From 51d96e879e4992355993f4cfa9997e7f60ecd85f Mon Sep 17 00:00:00 2001 From: Kelly Lockhart <2926089+kelockhart@users.noreply.github.com> Date: Wed, 2 Jul 2025 17:06:44 -0400 Subject: [PATCH 1/3] Added handling for MathML markup --- exportsrv/formatter/cslFormat.py | 5 ++ exportsrv/formatter/fieldedFormat.py | 4 +- exportsrv/formatter/rssFormat.py | 5 +- exportsrv/formatter/toLaTex.py | 61 ++++++++++++++++++- exportsrv/formatter/voTableFormat.py | 3 +- exportsrv/formatter/xmlFormat.py | 14 ++--- .../tests/unittests/stubdata/bibTexTest.py | 4 +- exportsrv/tests/unittests/stubdata/cslTest.py | 24 ++++---- .../tests/unittests/stubdata/customTest.py | 2 +- .../tests/unittests/stubdata/fieldedTest.py | 12 ++-- exportsrv/tests/unittests/stubdata/rssTest.py | 2 +- .../tests/unittests/stubdata/solrdata.py | 39 +++++++++++- .../tests/unittests/stubdata/voTableTest.py | 2 +- exportsrv/tests/unittests/stubdata/xmlTest.py | 10 +-- .../tests/unittests/test_export_service.py | 4 ++ exportsrv/tests/unittests/test_solrdata.py | 4 +- exportsrv/utils.py | 31 ++++++++++ 17 files changed, 183 insertions(+), 43 deletions(-) diff --git a/exportsrv/formatter/cslFormat.py b/exportsrv/formatter/cslFormat.py index 0d3a187..2df23fe 100755 --- a/exportsrv/formatter/cslFormat.py +++ b/exportsrv/formatter/cslFormat.py @@ -11,6 +11,7 @@ from exportsrv.formatter.format import Format from exportsrv.formatter.ads import adsFormatter, adsOrganizer, adsJournalFormat, adsOutputFormat from exportsrv.formatter.toLaTex import encode_laTex, encode_laTex_author, html_to_laTex, encode_latex_doi +from exportsrv.utils import mathml_to_plaintext # This class accepts JSON and sends it to citeproc library to get reformated # We are supporting, as of end of 2024, 11 complete cls (formatting all the fields) and 20 syles that @@ -146,6 +147,10 @@ def __update_data(self): for data in self.for_cls: if len(data.get('DOI', '')) > 0: data['DOI'] = data['DOI'].lstrip('doi:') + # remove MathML markup + elif (self.csl_style == 'ieee'): + for data in self.for_cls: + data['title'] = mathml_to_plaintext(data['title']) def __update_author_etal(self, author, the_rest, bibcode): diff --git a/exportsrv/formatter/fieldedFormat.py b/exportsrv/formatter/fieldedFormat.py index de8d4b3..91f10cf 100755 --- a/exportsrv/formatter/fieldedFormat.py +++ b/exportsrv/formatter/fieldedFormat.py @@ -9,7 +9,7 @@ from exportsrv.formatter.format import Format from exportsrv.formatter.ads import adsOutputFormat -from exportsrv.utils import get_eprint +from exportsrv.utils import get_eprint, mathml_to_plaintext from exportsrv.formatter.strftime import strftime # This class accepts JSON object created by Solr and can reformats it @@ -134,6 +134,7 @@ def __format_line_wrapped(self, text): return fill(text, width=72) + def __get_tags(self, export_format): """ convert from solr to each fielded types' tags @@ -537,6 +538,7 @@ def __add_in(self, field, value): """ if ((isinstance(value, str) or isinstance(value, bytes)) and (len(value) > 0)) or \ (isinstance(value, int) and (value is not None)): + value = mathml_to_plaintext(value) return field + ' ' + value + '\n' return '' diff --git a/exportsrv/formatter/rssFormat.py b/exportsrv/formatter/rssFormat.py index 566299b..a8ef504 100644 --- a/exportsrv/formatter/rssFormat.py +++ b/exportsrv/formatter/rssFormat.py @@ -7,6 +7,7 @@ from exportsrv.formatter.format import Format from exportsrv.formatter.ads import adsOutputFormat +from exportsrv.utils import mathml_to_plaintext class RSSFormat(Format): @@ -37,7 +38,7 @@ def __get_author_title(self, a_doc): first_author = '' if 'author' in a_doc: first_author = a_doc['author'][0] - title = ''.join(a_doc.get('title', '')) + title = mathml_to_plaintext(''.join(a_doc.get('title', ''))) if len(first_author) > 0 and len(title) > 0: return first_author + ': ' + title if len(first_author) > 0: @@ -87,7 +88,7 @@ def __get_doc(self, index): elif (field == 'url'): self.__add_in(item, fields[field], current_app.config.get('EXPORT_SERVICE_FROM_BBB_URL') + '/' + a_doc.get('bibcode', '')) elif (field == 'abstract'): - self.__add_in(item, fields[field], self.__format_line_wrapped(a_doc.get(field, ''))) + self.__add_in(item, fields[field], self.__format_line_wrapped(mathml_to_plaintext(a_doc.get(field, '')))) return item diff --git a/exportsrv/formatter/toLaTex.py b/exportsrv/formatter/toLaTex.py index 8593400..4c6d255 100755 --- a/exportsrv/formatter/toLaTex.py +++ b/exportsrv/formatter/toLaTex.py @@ -3,6 +3,7 @@ import re from collections import OrderedDict from exportsrv.formatter.latexencode import utf8tolatex +from lxml import etree # this module contains methods to encode for latex output @@ -34,6 +35,9 @@ def encode_laTex(text): :return: """ if (len(text) > 1): + # first remove/convert any mathML markup + text = mathml_to_latex(text) + # if any greek letter macro map it here # convert something like \\Sigma\\ to \textbackslash{}Sigma\textbackslash{} # however needs to go through utf8tolatex so add placeholder to be replaced afterward @@ -113,4 +117,59 @@ def html_to_laTex(text): """ for key in REGEX_HTML_TAG.keys(): text = key.sub(REGEX_HTML_TAG[key], text) - return text \ No newline at end of file + return text + + +def convert_mathml_element(el): + if not isinstance(el, etree._Element): + return "" + + tag = etree.QName(el).localname + + if tag == "msup": + base = convert_mathml_element(el[0]).strip() or "{}" + exp = convert_mathml_element(el[1]).strip() + return f"{base}$^{{{exp}}}$" + + if tag == "msub": + base = convert_mathml_element(el[0]).strip() or "{}" + sub = convert_mathml_element(el[1]).strip() + return f"{base}$_{{{sub}}}$" + + if tag == "mn" or tag == "mi": + return "".join(el.itertext()).strip() + + if tag == "mrow": + return "".join([convert_mathml_element(child) for child in el]) + + # fallback + return "".join(el.itertext()).strip() + +def mathml_to_latex(text): + # Regex to find ... blocks + pattern = re.compile(r"", re.DOTALL) + + def replace_mathml(match): + chunk = match.group(0) + # Clean the chunk so it's parseable + cleaned = ( + chunk + # have to squish the mathML markup into an XML format for lxml to work + .replace("", "") + .replace("``", "\"").replace("''", "\"") + ) + + parser = etree.XMLParser(recover=True) + try: + root = etree.fromstring(cleaned.encode(), parser=parser) + mml_math = root.xpath(".//*[local-name()='math']") # this will return an array + if mml_math: + return convert_mathml_element(mml_math[0]) + else: + return "[MATHML]" + except Exception as e: + return "[MATHML_ERROR]" + + # Substitute all MathML chunks with LaTeX equivalents + return pattern.sub(replace_mathml, text) diff --git a/exportsrv/formatter/voTableFormat.py b/exportsrv/formatter/voTableFormat.py index d7ed2b1..876e694 100644 --- a/exportsrv/formatter/voTableFormat.py +++ b/exportsrv/formatter/voTableFormat.py @@ -7,6 +7,7 @@ from exportsrv.formatter.format import Format from exportsrv.formatter.ads import adsOutputFormat from exportsrv.formatter.strftime import strftime +from exportsrv.utils import mathml_to_plaintext class VOTableFormat(Format): @@ -78,7 +79,7 @@ def __get_doc(self, index): if (field == 'bibcode'): self.__add_in_table_data(item, a_doc.get(field, '')) elif (field == 'title'): - self.__add_in_table_data(item, ''.join(a_doc.get(field, ''))) + self.__add_in_table_data(item, mathml_to_plaintext(''.join(a_doc.get(field, '')))) elif (field == 'author'): self.__add_in_table_data(item, '; '.join(a_doc.get(field, ''))) elif (field == 'pub_raw'): diff --git a/exportsrv/formatter/xmlFormat.py b/exportsrv/formatter/xmlFormat.py index 997acaa..7a43544 100755 --- a/exportsrv/formatter/xmlFormat.py +++ b/exportsrv/formatter/xmlFormat.py @@ -9,7 +9,7 @@ from exportsrv.formatter.format import Format from exportsrv.formatter.ads import adsOutputFormat -from exportsrv.utils import get_eprint +from exportsrv.utils import get_eprint, mathml_to_plaintext from exportsrv.formatter.strftime import strftime # This class accepts JSON object created by Solr and can reformat it @@ -481,7 +481,7 @@ def __get_doc_dublin_xml(self, index): if field in ['bibcode', 'copyright']: self.__add_in(record, fields[field], a_doc.get(field, '')) elif (field == 'title'): - self.__add_in(record, fields[field], ''.join(a_doc.get(field, ''))) + self.__add_in(record, fields[field], mathml_to_plaintext(''.join(a_doc.get(field, '')))) elif (field == 'author'): self.__add_author_list(a_doc, record, fields[field]) elif (field == 'pub_raw'): @@ -493,7 +493,7 @@ def __get_doc_dublin_xml(self, index): elif (field == 'url'): self.__add_in(record, fields[field], current_app.config.get('EXPORT_SERVICE_FROM_BBB_URL') + '/' + a_doc.get('bibcode', '')) elif (field == 'abstract'): - self.__add_in(record, fields[field], self.__format_line_wrapped(a_doc.get(field, ''))) + self.__add_in(record, fields[field], self.__format_line_wrapped(mathml_to_plaintext(a_doc.get(field, '')))) elif (field == 'doi'): self.__add_in(record, fields[field], self.__get_doi('; '.join(a_doc.get(field, '')))) elif (field == 'num_citations'): @@ -525,7 +525,7 @@ def __get_doc_reference_xml(self, index, xml_export_format): if field in ['bibcode', 'pub', 'volume', 'copyright']: self.__add_in(record, fields[field], a_doc.get(field, '')) elif field in ['title', 'doi']: - self.__add_in(record, fields[field], ''.join(a_doc.get(field, ''))) + self.__add_in(record, fields[field], mathml_to_plaintext(''.join(a_doc.get(field, '')))) elif (field == 'author'): self.__add_author_list(a_doc, record, fields[field]) elif (field == 'aff'): @@ -543,7 +543,7 @@ def __get_doc_reference_xml(self, index, xml_export_format): elif (field == 'num_citations'): self.__add_in(record, fields[field], self.__get_citation(int(a_doc.get(field, 0)), xml_export_format)) elif (field == 'abstract'): - self.__add_in(record, fields[field], self.__format_line_wrapped(a_doc.get(field, ''))) + self.__add_in(record, fields[field], self.__format_line_wrapped(mathml_to_plaintext(a_doc.get(field, '')))) elif (field == 'link'): self.__add_doc_links(a_doc, record) elif (field == 'eprintid'): @@ -705,7 +705,7 @@ def __get_doc_jats_xml(self, index): ET.SubElement(article_meta_section, fields[field], {"pub-id-type": "doi"}).text = '; '.join(a_doc.get(field, '')) elif (field == 'title'): title = ET.SubElement(article_meta_section, fields[field]) - ET.SubElement(title, 'article-title').text = '; '.join(a_doc.get(field, '')) + ET.SubElement(title, 'article-title').text = mathml_to_plaintext('; '.join(a_doc.get(field, ''))) elif (field == 'author'): # add `contrib-group` tag and call the function to add list of authors to this tag self.__add_author_list_jats_xml(a_doc, ET.SubElement(article_meta_section, fields[field])) @@ -719,7 +719,7 @@ def __get_doc_jats_xml(self, index): ET.SubElement(article_meta_section, "permissions").text = "" # add abstract tag, then paragraph tag around the abstract (required) abstract = ET.SubElement(article_meta_section, fields[field]) - self.__add_in(abstract, "p", a_doc.get(field, '')) + self.__add_in(abstract, "p", mathml_to_plaintext(a_doc.get(field, ''))) elif field in ['page', 'page_range']: self.__add_page(a_doc, article_meta_section, fields[field]) diff --git a/exportsrv/tests/unittests/stubdata/bibTexTest.py b/exportsrv/tests/unittests/stubdata/bibTexTest.py index 60ec1ef..151e763 100644 --- a/exportsrv/tests/unittests/stubdata/bibTexTest.py +++ b/exportsrv/tests/unittests/stubdata/bibTexTest.py @@ -1,8 +1,8 @@ # -*- coding: utf-8 -*- -data = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '@ARTICLE{2018Wthr...73Q..35.,\n title = "{Book reviews}",\n journal = {Weather},\n year = 2018,\n month = jan,\n volume = {73},\n number = {1},\n pages = {35-35},\n doi = {10.1002/wea.3072},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018TDM.....5a0201F,\n author = {{Fal\'ko}, Vladimir and {Thomas}, Ceri-Wyn},\n title = "{2D Materials: maintaining editorial quality}",\n journal = {2D Materials},\n year = 2018,\n month = jan,\n volume = {5},\n number = {1},\n eid = {010201},\n pages = {010201},\n doi = {10.1088/2053-1583/aa9403},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018Spin....877001P,\n author = {{Parkin}, Stuart and {Chantrell}, Roy and {Chang}, Ching-Ray},\n title = "{Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor}",\n journal = {Spin},\n year = 2018,\n month = jan,\n volume = {8},\n number = {4},\n eid = {1877001},\n pages = {1877001},\n doi = {10.1142/S2010324718770015},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018Spin....877001P},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2018SAAS...38.....D,\n author = {{Dessauges-Zavadsky}, Miroslava and {Pfenniger}, Daniel},\n title = "{Millimeter Astronomy}",\n keywords = {Physics},\n howpublished = {Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018},\n year = 2018,\n month = jan,\n doi = {10.1007/978-3-662-57546-8},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018PhRvL.120b9901P,\n author = {{Pustilnik}, M. and {van Heck}, B. and {Lutchyn}, R.~M. and {Glazman}, L.~I.},\n title = "{Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]}",\n journal = {\\prl},\n year = 2018,\n month = jan,\n volume = {120},\n number = {2},\n eid = {029901},\n pages = {029901},\n doi = {10.1103/PhysRevLett.120.029901},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PHDTHESIS{2017PhDT........14C,\n author = {{Carton}, David},\n title = "{Resolving Gas-Phase Metallicity In Galaxies}",\n keywords = {galaxies: evolution, galaxies: abundances, galaxies: ISM},\n school = {Leiden University},\n year = 2017,\n month = jun,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017PhDT........14C},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2017nova.pres.2388K,\n author = {{Kohler}, Susanna},\n title = "{A 3D View of a Supernova Remnant}",\n keywords = {Features, Highlights, interstellar medium, stellar evolution, supernova remnant, supernovae, white dwarfs},\n howpublished = {AAS Nova Highlight, 14 Jun 2017, id.2388},\n year = 2017,\n month = jun,\n eid = {2388},\n pages = {2388},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017CBET.4403....2G,\n author = {{Green}, D.~W.~E.},\n title = "{Potential New Meteor Shower from Comet C/2015 D4 (Borisov)}",\n journal = {Central Bureau Electronic Telegrams},\n year = 2017,\n month = jun,\n volume = {4403},\n pages = {2},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@software{2017ascl.soft06009C,\n author = {{Casey}, Andrew R.},\n title = "{sick: Spectroscopic inference crank}",\n howpublished = {Astrophysics Source Code Library, record ascl:1706.009},\n year = 2017,\n month = jun,\n eid = {ascl:1706.009},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017yCat.113380453S,\n author = {{Siltala}, J. and {Jetsu}, L. and {Hackman}, T. and {Henry}, G.~W. and {Immonen}, L. and {Kajatkari}, P. and {Lankinen}, J. and {Lehtinen}, J. and {Monira}, S. and {Nikbakhsh}, S. and {Viitanen}, A. and {Viuho}, J. and {Willamo}, T.},\n title = "{VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)}",\n journal = {VizieR Online Data Catalog},\n keywords = {Stars: variable},\n year = 2017,\n month = may,\n eid = {J/AN/338/453},\n pages = {J/AN/338/453},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017AAVSN.429....1W,\n author = {{Waagen}, Elizabeth O.},\n title = "{V694 Mon (MWC 560) spectroscopy requested}",\n journal = {AAVSO Special Notice},\n keywords = {astronomical databases: miscellaneous, binaries: symbiotic, stars: individual (V694 Mon, MWC 560)},\n year = 2017,\n month = may,\n volume = {429},\n pages = {1},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2017sptz.prop13168Y,\n author = {{Yan}, Lin},\n title = "{Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves}",\n howpublished = {Spitzer Proposal ID 13168},\n year = 2017,\n month = apr,\n pages = {13168},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MASTERSTHESIS{2017MsT..........2A,\n author = {{Azankpo}, Severin},\n title = "{Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope}",\n school = {University of Stellenbosch},\n year = 2017,\n month = mar,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017MsT..........2A},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2016emo6.rept.....R,\n author = {{Rotaru}, Adrian and {Pteancu}, Mircea and {Zaharia}, Cristian},\n title = "{The penumbral Moon\'s eclipse form 16 september 2016}",\n keywords = {THE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY},\n howpublished = {http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian)},\n year = 2016,\n month = oct,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2016iac..talk..872V,\n author = {{Velasco}, Sergio},\n title = "{Living on the edge: Adaptive Optics+Lucky Imaging}",\n howpublished = {IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof{\\\'\\i}sica de Canarias, 872},\n year = 2016,\n month = mar,\n pages = {872},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INCOLLECTION{2009bcet.book...65L,\n author = {{Liu}, Corey W. and {Alekseyev}, Viktor Y. and {Allwardt}, Jeffrey R. and {Bankovich}, Alexander J. and {Cade-Menun}, Barbara J. and {Davis}, Ronald W. and {Du}, Lin-Shu and {Garcia}, K. Christopher and {Herschlag}, Daniel and {Khosla}, Chaitan and {Kraut}, Daniel A. and {Li}, Qing and {Null}, Brian and {Puglisi}, Joseph D. and {Sigala}, Paul A. and {Stebbins}, Jonathan F. and {Varani}, Luca},\n title = "{The Diversity of Nuclear Magnetic Resonance Spectroscopy}",\n keywords = {Physics},\n booktitle = {Biophysics and the Challenges of Emerging Threats},\n year = 2009,\n editor = {{Puglisi}, Joseph D.},\n pages = {65},\n doi = {10.1007/978-90-481-2368-1_5},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{2007AAS...210.2104M,\n author = {{Mahabal}, Ashish A. and {Drake}, A.~J. and {Djorgovski}, S.~G. and {Donalek}, C. and {Glikman}, E. and {Graham}, M.~J. and {Williams}, R. and {Baltay}, C. and {Rabinowitz}, D. and {PQ Team Caltech} and {Yale} and {NCSA} and {Indiana} and {}, . . .},\n title = "{Time Domain Exploration with the Palomar-QUEST Sky Survey}",\n booktitle = {American Astronomical Society Meeting Abstracts \\#210},\n year = 2007,\n series = {American Astronomical Society Meeting Abstracts},\n volume = {210},\n month = may,\n eid = {21.04},\n pages = {21.04},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2007RJPh....1...35.,\n author = {{.}, S.~N. Agbo and {.}, E.~C. Okoroigwe},\n title = "{Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater}",\n journal = {Research Journal of Physics},\n year = 2007,\n month = jan,\n volume = {1},\n number = {1},\n pages = {35-41},\n doi = {10.3923/rjp.2007.35.41},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{1995ans..agar..390M,\n author = {{Miller}, Judy L.},\n title = "{Spacecraft navigation requirements}",\n keywords = {Earth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space Navigation, Spacecraft Trajectories, Support Systems, Technology Assessment, Technology Utilization, Ascent Trajectories, Reentry Trajectories, Spacecraft, Spacecraft Performance, Spacecraft Survivability, Tradeoffs, Weight (Mass), Space Communications, Spacecraft Communications, Command and Tracking},\n booktitle = {In AGARD},\n year = 1995,\n month = jun,\n pages = {390-405},\n adsurl = {https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@BOOK{1995anda.book.....N,\n author = {{Nayfeh}, Ali H. and {Balachandran}, Balakumar},\n title = "{Applied nonlinear dynamics: analytical, computational and experimental methods}",\n year = 1995,\n adsurl = {https://ui.adsabs.harvard.edu/abs/1995anda.book.....N},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{1991hep.th....8028G,\n author = {{Ginsparg}, Paul},\n title = "{Applied Conformal Field Theory}",\n journal = {arXiv e-prints},\n keywords = {High Energy Physics - Theory},\n year = 1988,\n month = nov,\n eid = {hep-th/9108028},\n pages = {hep-th/9108028},\narchivePrefix = {arXiv},\n eprint = {hep-th/9108028},\n primaryClass = {hep-th},\n adsurl = {https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PROCEEDINGS{1983aiaa.meetY....K,\n title = "{Autonomous navigation using lunar beacons}",\n keywords = {Artificial Satellites, Autonomous Navigation, Earth-Moon System, Lunar Communication, Radio Beacons, Radio Navigation, Space Navigation, Doppler Navigation, Least Squares Method, Orbit Calculation, Space Communications, Spacecraft Communications, Command and Tracking},\n booktitle = {AIAA, Aerospace Sciences Meeting},\n year = 1983,\n month = jan,\n adsurl = {https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@dataset{2012ddsw.rept.....T,\n author = {{Thornton}, P.~E. and {Thornton}, M.~M. and {Mayer}, B.~W. and {Wilhelmi}, N. and {Wei}, Y. and {Devarakonda}, R. and {Cook}, R.},\n title = "{Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008}",\n howpublished = {Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)},\n year = 2012,\n month = apr,\n doi = {10.3334/ORNLDAAC/1219},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n'} +data = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '@ARTICLE{2018Wthr...73Q..35.,\n title = "{Book reviews}",\n journal = {Weather},\n year = 2018,\n month = jan,\n volume = {73},\n number = {1},\n pages = {35-35},\n doi = {10.1002/wea.3072},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018TDM.....5a0201F,\n author = {{Fal\'ko}, Vladimir and {Thomas}, Ceri-Wyn},\n title = "{2D Materials: maintaining editorial quality}",\n journal = {2D Materials},\n year = 2018,\n month = jan,\n volume = {5},\n number = {1},\n eid = {010201},\n pages = {010201},\n doi = {10.1088/2053-1583/aa9403},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018Spin....877001P,\n author = {{Parkin}, Stuart and {Chantrell}, Roy and {Chang}, Ching-Ray},\n title = "{Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor}",\n journal = {Spin},\n year = 2018,\n month = jan,\n volume = {8},\n number = {4},\n eid = {1877001},\n pages = {1877001},\n doi = {10.1142/S2010324718770015},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018Spin....877001P},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2018SAAS...38.....D,\n author = {{Dessauges-Zavadsky}, Miroslava and {Pfenniger}, Daniel},\n title = "{Millimeter Astronomy}",\n keywords = {Physics},\n howpublished = {Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018},\n year = 2018,\n month = jan,\n doi = {10.1007/978-3-662-57546-8},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018PhRvL.120b9901P,\n author = {{Pustilnik}, M. and {van Heck}, B. and {Lutchyn}, R.~M. and {Glazman}, L.~I.},\n title = "{Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]}",\n journal = {\\prl},\n year = 2018,\n month = jan,\n volume = {120},\n number = {2},\n eid = {029901},\n pages = {029901},\n doi = {10.1103/PhysRevLett.120.029901},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PHDTHESIS{2017PhDT........14C,\n author = {{Carton}, David},\n title = "{Resolving Gas-Phase Metallicity In Galaxies}",\n keywords = {galaxies: evolution, galaxies: abundances, galaxies: ISM},\n school = {Leiden University},\n year = 2017,\n month = jun,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017PhDT........14C},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2017nova.pres.2388K,\n author = {{Kohler}, Susanna},\n title = "{A 3D View of a Supernova Remnant}",\n keywords = {Features, Highlights, interstellar medium, stellar evolution, supernova remnant, supernovae, white dwarfs},\n howpublished = {AAS Nova Highlight, 14 Jun 2017, id.2388},\n year = 2017,\n month = jun,\n eid = {2388},\n pages = {2388},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017CBET.4403....2G,\n author = {{Green}, D.~W.~E.},\n title = "{Potential New Meteor Shower from Comet C/2015 D4 (Borisov)}",\n journal = {Central Bureau Electronic Telegrams},\n year = 2017,\n month = jun,\n volume = {4403},\n pages = {2},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@software{2017ascl.soft06009C,\n author = {{Casey}, Andrew R.},\n title = "{sick: Spectroscopic inference crank}",\n howpublished = {Astrophysics Source Code Library, record ascl:1706.009},\n year = 2017,\n month = jun,\n eid = {ascl:1706.009},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017yCat.113380453S,\n author = {{Siltala}, J. and {Jetsu}, L. and {Hackman}, T. and {Henry}, G.~W. and {Immonen}, L. and {Kajatkari}, P. and {Lankinen}, J. and {Lehtinen}, J. and {Monira}, S. and {Nikbakhsh}, S. and {Viitanen}, A. and {Viuho}, J. and {Willamo}, T.},\n title = "{VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)}",\n journal = {VizieR Online Data Catalog},\n keywords = {Stars: variable},\n year = 2017,\n month = may,\n eid = {J/AN/338/453},\n pages = {J/AN/338/453},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017AAVSN.429....1W,\n author = {{Waagen}, Elizabeth O.},\n title = "{V694 Mon (MWC 560) spectroscopy requested}",\n journal = {AAVSO Special Notice},\n keywords = {astronomical databases: miscellaneous, binaries: symbiotic, stars: individual (V694 Mon, MWC 560)},\n year = 2017,\n month = may,\n volume = {429},\n pages = {1},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2017sptz.prop13168Y,\n author = {{Yan}, Lin},\n title = "{Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves}",\n howpublished = {Spitzer Proposal ID 13168},\n year = 2017,\n month = apr,\n pages = {13168},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MASTERSTHESIS{2017MsT..........2A,\n author = {{Azankpo}, Severin},\n title = "{Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope}",\n school = {University of Stellenbosch},\n year = 2017,\n month = mar,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017MsT..........2A},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2016emo6.rept.....R,\n author = {{Rotaru}, Adrian and {Pteancu}, Mircea and {Zaharia}, Cristian},\n title = "{The penumbral Moon\'s eclipse form 16 september 2016}",\n keywords = {THE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY},\n howpublished = {http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian)},\n year = 2016,\n month = oct,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2016iac..talk..872V,\n author = {{Velasco}, Sergio},\n title = "{Living on the edge: Adaptive Optics+Lucky Imaging}",\n howpublished = {IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof{\\\'\\i}sica de Canarias, 872},\n year = 2016,\n month = mar,\n pages = {872},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INCOLLECTION{2009bcet.book...65L,\n author = {{Liu}, Corey W. and {Alekseyev}, Viktor Y. and {Allwardt}, Jeffrey R. and {Bankovich}, Alexander J. and {Cade-Menun}, Barbara J. and {Davis}, Ronald W. and {Du}, Lin-Shu and {Garcia}, K. Christopher and {Herschlag}, Daniel and {Khosla}, Chaitan and {Kraut}, Daniel A. and {Li}, Qing and {Null}, Brian and {Puglisi}, Joseph D. and {Sigala}, Paul A. and {Stebbins}, Jonathan F. and {Varani}, Luca},\n title = "{The Diversity of Nuclear Magnetic Resonance Spectroscopy}",\n keywords = {Physics},\n booktitle = {Biophysics and the Challenges of Emerging Threats},\n year = 2009,\n editor = {{Puglisi}, Joseph D.},\n pages = {65},\n doi = {10.1007/978-90-481-2368-1_5},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{2007AAS...210.2104M,\n author = {{Mahabal}, Ashish A. and {Drake}, A.~J. and {Djorgovski}, S.~G. and {Donalek}, C. and {Glikman}, E. and {Graham}, M.~J. and {Williams}, R. and {Baltay}, C. and {Rabinowitz}, D. and {PQ Team Caltech} and {Yale} and {NCSA} and {Indiana} and {}, . . .},\n title = "{Time Domain Exploration with the Palomar-QUEST Sky Survey}",\n booktitle = {American Astronomical Society Meeting Abstracts \\#210},\n year = 2007,\n series = {American Astronomical Society Meeting Abstracts},\n volume = {210},\n month = may,\n eid = {21.04},\n pages = {21.04},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2007RJPh....1...35.,\n author = {{.}, S.~N. Agbo and {.}, E.~C. Okoroigwe},\n title = "{Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater}",\n journal = {Research Journal of Physics},\n year = 2007,\n month = jan,\n volume = {1},\n number = {1},\n pages = {35-41},\n doi = {10.3923/rjp.2007.35.41},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{1995ans..agar..390M,\n author = {{Miller}, Judy L.},\n title = "{Spacecraft navigation requirements}",\n keywords = {Earth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space Navigation, Spacecraft Trajectories, Support Systems, Technology Assessment, Technology Utilization, Ascent Trajectories, Reentry Trajectories, Spacecraft, Spacecraft Performance, Spacecraft Survivability, Tradeoffs, Weight (Mass), Space Communications, Spacecraft Communications, Command and Tracking},\n booktitle = {In AGARD},\n year = 1995,\n month = jun,\n pages = {390-405},\n adsurl = {https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@BOOK{1995anda.book.....N,\n author = {{Nayfeh}, Ali H. and {Balachandran}, Balakumar},\n title = "{Applied nonlinear dynamics: analytical, computational and experimental methods}",\n year = 1995,\n adsurl = {https://ui.adsabs.harvard.edu/abs/1995anda.book.....N},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{1991hep.th....8028G,\n author = {{Ginsparg}, Paul},\n title = "{Applied Conformal Field Theory}",\n journal = {arXiv e-prints},\n keywords = {High Energy Physics - Theory},\n year = 1988,\n month = nov,\n eid = {hep-th/9108028},\n pages = {hep-th/9108028},\narchivePrefix = {arXiv},\n eprint = {hep-th/9108028},\n primaryClass = {hep-th},\n adsurl = {https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PROCEEDINGS{1983aiaa.meetY....K,\n title = "{Autonomous navigation using lunar beacons}",\n keywords = {Artificial Satellites, Autonomous Navigation, Earth-Moon System, Lunar Communication, Radio Beacons, Radio Navigation, Space Navigation, Doppler Navigation, Least Squares Method, Orbit Calculation, Space Communications, Spacecraft Communications, Command and Tracking},\n booktitle = {AIAA, Aerospace Sciences Meeting},\n year = 1983,\n month = jan,\n adsurl = {https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@dataset{2012ddsw.rept.....T,\n author = {{Thornton}, P.~E. and {Thornton}, M.~M. and {Mayer}, B.~W. and {Wilhelmi}, N. and {Wei}, Y. and {Devarakonda}, R. and {Cook}, R.},\n title = "{Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008}",\n howpublished = {Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)},\n year = 2012,\n month = apr,\n doi = {10.3334/ORNLDAAC/1219},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2020EPJC...80...96D,\n author = {{Dhaygude}, Akanksha and {Desai}, Shantanu},\n title = "{Generalized Lomb{\\textendash}Scargle analysis of 36Cl decay rate measurements at PTB and BNL}",\n journal = {European Physical Journal C},\n keywords = {Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Nuclear Experiment},\n year = 2020,\n month = feb,\n doi = {10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970},\narchivePrefix = {arXiv},\n eprint = {1912.06970},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n'} -data_with_abs= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '@ARTICLE{2018Wthr...73Q..35.,\n title = "{Book reviews}",\n journal = {Weather},\n year = 2018,\n month = jan,\n volume = {73},\n number = {1},\n pages = {35-35},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.1002/wea.3072},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018TDM.....5a0201F,\n author = {{Fal\'ko}, Vladimir and {Thomas}, Ceri-Wyn},\n title = "{2D Materials: maintaining editorial quality}",\n journal = {2D Materials},\n year = 2018,\n month = jan,\n volume = {5},\n number = {1},\n eid = {010201},\n pages = {010201},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.1088/2053-1583/aa9403},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018Spin....877001P,\n author = {{Parkin}, Stuart and {Chantrell}, Roy and {Chang}, Ching-Ray},\n title = "{Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor}",\n journal = {Spin},\n year = 2018,\n month = jan,\n volume = {8},\n number = {4},\n eid = {1877001},\n pages = {1877001},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.1142/S2010324718770015},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018Spin....877001P},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2018SAAS...38.....D,\n author = {{Dessauges-Zavadsky}, Miroslava and {Pfenniger}, Daniel},\n title = "{Millimeter Astronomy}",\n keywords = {Physics},\n howpublished = {Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018},\n year = 2018,\n month = jan,\n doi = {10.1007/978-3-662-57546-8},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018PhRvL.120b9901P,\n author = {{Pustilnik}, M. and {van Heck}, B. and {Lutchyn}, R.~M. and {Glazman}, L.~I.},\n title = "{Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]}",\n journal = {\\prl},\n year = 2018,\n month = jan,\n volume = {120},\n number = {2},\n eid = {029901},\n pages = {029901},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.1103/PhysRevLett.120.029901},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PHDTHESIS{2017PhDT........14C,\n author = {{Carton}, David},\n title = "{Resolving Gas-Phase Metallicity In Galaxies}",\n keywords = {galaxies: evolution, galaxies: abundances, galaxies: ISM},\n school = {Leiden University},\n year = 2017,\n month = jun,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017PhDT........14C},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2017nova.pres.2388K,\n author = {{Kohler}, Susanna},\n title = "{A 3D View of a Supernova Remnant}",\n keywords = {Features, Highlights, interstellar medium, stellar evolution, supernova remnant, supernovae, white dwarfs},\n howpublished = {AAS Nova Highlight, 14 Jun 2017, id.2388},\n year = 2017,\n month = jun,\n eid = {2388},\n pages = {2388},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017CBET.4403....2G,\n author = {{Green}, D.~W.~E.},\n title = "{Potential New Meteor Shower from Comet C/2015 D4 (Borisov)}",\n journal = {Central Bureau Electronic Telegrams},\n year = 2017,\n month = jun,\n volume = {4403},\n pages = {2},\n abstract = "{A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta\n = +0.0003 AU, solar long. = 125.841 deg). Future encounters are\n predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042\n July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m\n (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT\n (-0.0001 AU, 125.863 deg). \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@software{2017ascl.soft06009C,\n author = {{Casey}, Andrew R.},\n title = "{sick: Spectroscopic inference crank}",\n howpublished = {Astrophysics Source Code Library, record ascl:1706.009},\n year = 2017,\n month = jun,\n eid = {ascl:1706.009},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017yCat.113380453S,\n author = {{Siltala}, J. and {Jetsu}, L. and {Hackman}, T. and {Henry}, G.~W. and {Immonen}, L. and {Kajatkari}, P. and {Lankinen}, J. and {Lehtinen}, J. and {Monira}, S. and {Nikbakhsh}, S. and {Viitanen}, A. and {Viuho}, J. and {Willamo}, T.},\n title = "{VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)}",\n journal = {VizieR Online Data Catalog},\n keywords = {Stars: variable},\n year = 2017,\n month = may,\n eid = {J/AN/338/453},\n pages = {J/AN/338/453},\n abstract = "{The included files present the numerical data of our analysis of the BM\n CVn photometry. The data consists of differential Johnson V-band\n photometry using the star HD 116010 as the comparison star.\n \\textbackslash\\textbackslashThe analysis has been performed\n using the previously published continuous period search (CPS)\n method, described in detail in Lehtinen et al.,\n 2011A\\&A...527A.136L, Cat. J/A+A/527/A136.\n \\textbackslash\\textbackslash(4 data files).\n \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017AAVSN.429....1W,\n author = {{Waagen}, Elizabeth O.},\n title = "{V694 Mon (MWC 560) spectroscopy requested}",\n journal = {AAVSO Special Notice},\n keywords = {astronomical databases: miscellaneous, binaries: symbiotic, stars: individual (V694 Mon, MWC 560)},\n year = 2017,\n month = may,\n volume = {429},\n pages = {1},\n abstract = "{The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert\n Notice 538) has been continued, but with different requirements.\n Photometry is no longer specifically requested on a regular\n basis (although ongoing observations that do not interfere with\n other obligations are welcome). Spectroscopy on a cadence of a\n week or two is requested to monitor changes in the disk outflow.\n Investigator Adrian Lucy writes: ``Adrian Lucy and Dr. Jeno\n Sokoloski (Columbia University) have requested spectroscopic\n monitoring of the broad-absorption-line symbiotic star V694 Mon\n (MWC 560), as a follow-up to coordinated multi-wavelength\n observations obtained during its recent outburst (ATel \\#8653,\n \\#8832, \\#8957; \\#10281). This system is a perfect place in\n which to study the relationship between an accretion disk and\n disk winds/jets, and a high-value target for which even low-\n resolution spectra can be extraordinarily useful...Optical\n brightening in MWC 560 tends to predict higher-velocity\n absorption, but sometimes jumps in absorption velocity also\n appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242,\n 187). If such a velocity jump occurs during photometric\n quiescence, it may prompt radio observations to confirm and test\n the proposed outflow origin for recently-discovered flat-\n spectrum radio emission (Lucy et al. ATel\n \\#10281)...Furthermore, volunteer spectroscopic monitoring of\n this system has proved useful in unpredictable ways. For\n example, \'amateur\' spectra obtained by Somogyi P{\\\'e}ter in 2015\n December demonstrated that the velocity of absorption was very\n low only a month before an optical outburst peak prompted\n absorption troughs up to 3000 km/s, which constrains very well\n the timing of the changes to the outflow to a degree that would\n not have been otherwise possible. Any resolution can be useful.\n A wavelength range that can accommodate a blueshift of at least\n 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha\n at 6562 angstroms and/or H-beta at 4861 angstroms is ideal,\n though spectra with a smaller range can still be useful.\n Photometry could potentially still be useful, but will be\n supplementary to medium-cadence photometry being collected by\n the ANS collaboration.\'\' \'\'Spectroscopy may be uploaded to the\n ARAS database\n (http://www.astrosurf.com/aras/Aras\\_DataBase/DataBase.htm), or\n sent to Adrian and Jeno directly at\n $\\lt$lucy@astro.columbia.edu$\\gt$. Finder charts with sequence\n may be created using the AAVSO Variable Star Plotter\n (https://www.aavso.org/vsp). Photometry should be submitted to\n the AAVSO International Database. See full Special Notice for\n more details. \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2017sptz.prop13168Y,\n author = {{Yan}, Lin},\n title = "{Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves}",\n howpublished = {Spitzer Proposal ID 13168},\n year = 2017,\n month = apr,\n pages = {13168},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MASTERSTHESIS{2017MsT..........2A,\n author = {{Azankpo}, Severin},\n title = "{Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope}",\n school = {University of Stellenbosch},\n year = 2017,\n month = mar,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017MsT..........2A},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2016emo6.rept.....R,\n author = {{Rotaru}, Adrian and {Pteancu}, Mircea and {Zaharia}, Cristian},\n title = "{The penumbral Moon\'s eclipse form 16 september 2016}",\n keywords = {THE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY},\n howpublished = {http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian)},\n year = 2016,\n month = oct,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2016iac..talk..872V,\n author = {{Velasco}, Sergio},\n title = "{Living on the edge: Adaptive Optics+Lucky Imaging}",\n howpublished = {IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof{\\\'\\i}sica de Canarias, 872},\n year = 2016,\n month = mar,\n pages = {872},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INCOLLECTION{2009bcet.book...65L,\n author = {{Liu}, Corey W. and {Alekseyev}, Viktor Y. and {Allwardt}, Jeffrey R. and {Bankovich}, Alexander J. and {Cade-Menun}, Barbara J. and {Davis}, Ronald W. and {Du}, Lin-Shu and {Garcia}, K. Christopher and {Herschlag}, Daniel and {Khosla}, Chaitan and {Kraut}, Daniel A. and {Li}, Qing and {Null}, Brian and {Puglisi}, Joseph D. and {Sigala}, Paul A. and {Stebbins}, Jonathan F. and {Varani}, Luca},\n title = "{The Diversity of Nuclear Magnetic Resonance Spectroscopy}",\n keywords = {Physics},\n booktitle = {Biophysics and the Challenges of Emerging Threats},\n year = 2009,\n editor = {{Puglisi}, Joseph D.},\n pages = {65},\n abstract = "{The discovery of the physical phenomenon of Nuclear Magnetic Resonance\n (NMR) in 1946 gave rise to the spectroscopic technique that has\n become a remarkably versatile research tool. One could\n oversimplify NMR spectros-copy by categorizing it into the two\n broad applications of structure elucidation of molecules\n (associated with chemistry and biology) and imaging (associated\n with medicine). But, this certainly does not do NMR spectroscopy\n justice in demonstrating its general acceptance and utilization\n across the sciences. This manuscript is not an effort to present\n an exhaustive, or even partial review of NMR spectroscopy\n applications, but rather to provide a glimpse at the wide-\n ranging uses of NMR spectroscopy found within the confines of a\n single magnetic resonance research facility, the Stanford\n Magnetic Resonance Laboratory. Included here are summaries of\n projects involving protein structure determination, mapping of\n intermolecular interactions, exploring fundamental biological\n mechanisms, following compound cycling in the environmental,\n analysis of synthetic solid compounds, and microimaging of a\n model organism. \\textbackslash\\textbackslash}",\n doi = {10.1007/978-90-481-2368-1_5},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{2007AAS...210.2104M,\n author = {{Mahabal}, Ashish A. and {Drake}, A.~J. and {Djorgovski}, S.~G. and {Donalek}, C. and {Glikman}, E. and {Graham}, M.~J. and {Williams}, R. and {Baltay}, C. and {Rabinowitz}, D. and {PQ Team Caltech} and {Yale} and {NCSA} and {Indiana} and {}, . . .},\n title = "{Time Domain Exploration with the Palomar-QUEST Sky Survey}",\n booktitle = {American Astronomical Society Meeting Abstracts \\#210},\n year = 2007,\n series = {American Astronomical Society Meeting Abstracts},\n volume = {210},\n month = may,\n eid = {21.04},\n pages = {21.04},\n abstract = "{Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing\n data from driftscans in real-time. As four photometric\n bandpasses are utilized in nearly simultaneously, PQ is well\n suited to search for transient and highly variable objects.\n Using a series of software filters i.e. programs to\n select/deselect objects based on certain criteria we shorten the\n list of candidates from the initially flagged candidate\n transients. Such filters include looking for known asteroids,\n known variables, as well as moving, but previously uncatalogued\n objects based on their motion within a scan as well as between\n successive scans. Some software filters also deal with\n instrumental artifacts, edge effects, and use clustering of\n spurious detections around bright stars. During a typical night\n when we cover about 500 sq. degrees, we detect hundreds of\n asteroids, the primary contaminants in the search for\n astrophysical transients beyond our solar system.\n \\textbackslash\\textbackslashHere we describe some statistics\n based on the software filters we employ and the nature of the\n objects that seem to survive the process. We also discuss the\n usefulness of this to amateur astronomers, projects like\n VOEventNet, and other synoptic sky surveys.\n \\textbackslash\\textbackslashWe also present an outline of the\n work we have started on quantifying the variability of quasars,\n blazars, as well as various classes of Galactic sources, by\n combining the large number of PQ scans with other existing data\n sources federated in the Virtual Observatory environment.\n \\textbackslash\\textbackslashThe PQ survey is partially supported\n by the U.S. National Science Foundation (NSF).\n \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2007RJPh....1...35.,\n author = {{.}, S.~N. Agbo and {.}, E.~C. Okoroigwe},\n title = "{Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater}",\n journal = {Research Journal of Physics},\n year = 2007,\n month = jan,\n volume = {1},\n number = {1},\n pages = {35-41},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.3923/rjp.2007.35.41},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{1995ans..agar..390M,\n author = {{Miller}, Judy L.},\n title = "{Spacecraft navigation requirements}",\n keywords = {Earth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space Navigation, Spacecraft Trajectories, Support Systems, Technology Assessment, Technology Utilization, Ascent Trajectories, Reentry Trajectories, Spacecraft, Spacecraft Performance, Spacecraft Survivability, Tradeoffs, Weight (Mass), Space Communications, Spacecraft Communications, Command and Tracking},\n booktitle = {In AGARD},\n year = 1995,\n month = jun,\n pages = {390-405},\n abstract = "{Spacecraft operation depends upon knowledge of vehicular position and,\n consequently, navigational support has been required for all\n such systems. Technical requirements for different mission\n trajectories and orbits are addressed with consideration given\n to the various tradeoffs which may need to be considered. The\n broad spectrum of spacecraft are considered with emphasis upon\n those of greater military significance (i.e., near earth\n orbiting satellites). Technical requirements include, but are\n not limited to, accuracy; physical characteristics such as\n weight and volume; support requirements such as electrical power\n and ground support; and system integrity. Generic navigation\n suites for spacecraft applications are described. It is shown\n that operational spacecraft rely primarily upon ground-based\n tracking and computational centers with little or no\n navigational function allocated to the vehicle, while technology\n development efforts have been and continue to be directed\n primarily toward onboard navigation suites. The military\n significance of onboard navigators is shown to both improve\n spacecraft survivability and performance (accuracy).\n \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@BOOK{1995anda.book.....N,\n author = {{Nayfeh}, Ali H. and {Balachandran}, Balakumar},\n title = "{Applied nonlinear dynamics: analytical, computational and experimental methods}",\n year = 1995,\n adsurl = {https://ui.adsabs.harvard.edu/abs/1995anda.book.....N},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{1991hep.th....8028G,\n author = {{Ginsparg}, Paul},\n title = "{Applied Conformal Field Theory}",\n journal = {arXiv e-prints},\n keywords = {High Energy Physics - Theory},\n year = 1988,\n month = nov,\n eid = {hep-th/9108028},\n pages = {hep-th/9108028},\n abstract = "{These lectures consisted of an elementary introduction to conformal\n field theory, with some applications to statistical mechanical\n systems, and fewer to string theory. Contents: 1. Conformal\n theories in d dimensions 2. Conformal theories in 2 dimensions\n 3. The central charge and the Virasoro algebra 4. Kac\n determinant and unitarity 5. Identication of m = 3 with the\n critical Ising model 6. Free bosons and fermions 7. Free\n fermions on a torus 8. Free bosons on a torus 9. Affine Kac-\n Moody algebras and coset constructions 10. Advanced applications\n \\textbackslash\\textbackslash}",\narchivePrefix = {arXiv},\n eprint = {hep-th/9108028},\n primaryClass = {hep-th},\n adsurl = {https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PROCEEDINGS{1983aiaa.meetY....K,\n title = "{Autonomous navigation using lunar beacons}",\n keywords = {Artificial Satellites, Autonomous Navigation, Earth-Moon System, Lunar Communication, Radio Beacons, Radio Navigation, Space Navigation, Doppler Navigation, Least Squares Method, Orbit Calculation, Space Communications, Spacecraft Communications, Command and Tracking},\n booktitle = {AIAA, Aerospace Sciences Meeting},\n year = 1983,\n month = jan,\n abstract = "{The concept of using lunar beacon signal transmission for on-board\n navigation for earth satellites and near-earth spacecraft is\n described. The system would require powerful transmitters on the\n earth-side of the moon\'s surface and black box receivers with\n antennae and microprocessors placed on board spacecraft for\n autonomous navigation. Spacecraft navigation requires three\n position and three velocity elements to establish location\n coordinates. Two beacons could be soft-landed on the lunar\n surface at the limits of allowable separation and each would\n transmit a wide-beam signal with cones reaching GEO heights and\n be strong enough to be received by small antennae in near-earth\n orbit. The black box processor would perform on-board\n computation with one-way Doppler/range data and dynamical\n models. Alternatively, GEO satellites such as the GPS or TDRSS\n spacecraft can be used with interferometric techniques to\n provide decimeter-level accuracy for aircraft navigation.\n \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@dataset{2012ddsw.rept.....T,\n author = {{Thornton}, P.~E. and {Thornton}, M.~M. and {Mayer}, B.~W. and {Wilhelmi}, N. and {Wei}, Y. and {Devarakonda}, R. and {Cook}, R.},\n title = "{Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008}",\n howpublished = {Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)},\n year = 2012,\n month = apr,\n doi = {10.3334/ORNLDAAC/1219},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n'} +data_with_abs= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '@ARTICLE{2018Wthr...73Q..35.,\n title = "{Book reviews}",\n journal = {Weather},\n year = 2018,\n month = jan,\n volume = {73},\n number = {1},\n pages = {35-35},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.1002/wea.3072},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018TDM.....5a0201F,\n author = {{Fal\'ko}, Vladimir and {Thomas}, Ceri-Wyn},\n title = "{2D Materials: maintaining editorial quality}",\n journal = {2D Materials},\n year = 2018,\n month = jan,\n volume = {5},\n number = {1},\n eid = {010201},\n pages = {010201},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.1088/2053-1583/aa9403},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018Spin....877001P,\n author = {{Parkin}, Stuart and {Chantrell}, Roy and {Chang}, Ching-Ray},\n title = "{Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor}",\n journal = {Spin},\n year = 2018,\n month = jan,\n volume = {8},\n number = {4},\n eid = {1877001},\n pages = {1877001},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.1142/S2010324718770015},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018Spin....877001P},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2018SAAS...38.....D,\n author = {{Dessauges-Zavadsky}, Miroslava and {Pfenniger}, Daniel},\n title = "{Millimeter Astronomy}",\n keywords = {Physics},\n howpublished = {Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018},\n year = 2018,\n month = jan,\n doi = {10.1007/978-3-662-57546-8},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2018PhRvL.120b9901P,\n author = {{Pustilnik}, M. and {van Heck}, B. and {Lutchyn}, R.~M. and {Glazman}, L.~I.},\n title = "{Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]}",\n journal = {\\prl},\n year = 2018,\n month = jan,\n volume = {120},\n number = {2},\n eid = {029901},\n pages = {029901},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.1103/PhysRevLett.120.029901},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PHDTHESIS{2017PhDT........14C,\n author = {{Carton}, David},\n title = "{Resolving Gas-Phase Metallicity In Galaxies}",\n keywords = {galaxies: evolution, galaxies: abundances, galaxies: ISM},\n school = {Leiden University},\n year = 2017,\n month = jun,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017PhDT........14C},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2017nova.pres.2388K,\n author = {{Kohler}, Susanna},\n title = "{A 3D View of a Supernova Remnant}",\n keywords = {Features, Highlights, interstellar medium, stellar evolution, supernova remnant, supernovae, white dwarfs},\n howpublished = {AAS Nova Highlight, 14 Jun 2017, id.2388},\n year = 2017,\n month = jun,\n eid = {2388},\n pages = {2388},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017CBET.4403....2G,\n author = {{Green}, D.~W.~E.},\n title = "{Potential New Meteor Shower from Comet C/2015 D4 (Borisov)}",\n journal = {Central Bureau Electronic Telegrams},\n year = 2017,\n month = jun,\n volume = {4403},\n pages = {2},\n abstract = "{A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta\n = +0.0003 AU, solar long. = 125.841 deg). Future encounters are\n predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042\n July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m\n (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT\n (-0.0001 AU, 125.863 deg). \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@software{2017ascl.soft06009C,\n author = {{Casey}, Andrew R.},\n title = "{sick: Spectroscopic inference crank}",\n howpublished = {Astrophysics Source Code Library, record ascl:1706.009},\n year = 2017,\n month = jun,\n eid = {ascl:1706.009},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017yCat.113380453S,\n author = {{Siltala}, J. and {Jetsu}, L. and {Hackman}, T. and {Henry}, G.~W. and {Immonen}, L. and {Kajatkari}, P. and {Lankinen}, J. and {Lehtinen}, J. and {Monira}, S. and {Nikbakhsh}, S. and {Viitanen}, A. and {Viuho}, J. and {Willamo}, T.},\n title = "{VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)}",\n journal = {VizieR Online Data Catalog},\n keywords = {Stars: variable},\n year = 2017,\n month = may,\n eid = {J/AN/338/453},\n pages = {J/AN/338/453},\n abstract = "{The included files present the numerical data of our analysis of the BM\n CVn photometry. The data consists of differential Johnson V-band\n photometry using the star HD 116010 as the comparison star.\n \\textbackslash\\textbackslashThe analysis has been performed\n using the previously published continuous period search (CPS)\n method, described in detail in Lehtinen et al.,\n 2011A\\&A...527A.136L, Cat. J/A+A/527/A136.\n \\textbackslash\\textbackslash(4 data files).\n \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2017AAVSN.429....1W,\n author = {{Waagen}, Elizabeth O.},\n title = "{V694 Mon (MWC 560) spectroscopy requested}",\n journal = {AAVSO Special Notice},\n keywords = {astronomical databases: miscellaneous, binaries: symbiotic, stars: individual (V694 Mon, MWC 560)},\n year = 2017,\n month = may,\n volume = {429},\n pages = {1},\n abstract = "{The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert\n Notice 538) has been continued, but with different requirements.\n Photometry is no longer specifically requested on a regular\n basis (although ongoing observations that do not interfere with\n other obligations are welcome). Spectroscopy on a cadence of a\n week or two is requested to monitor changes in the disk outflow.\n Investigator Adrian Lucy writes: ``Adrian Lucy and Dr. Jeno\n Sokoloski (Columbia University) have requested spectroscopic\n monitoring of the broad-absorption-line symbiotic star V694 Mon\n (MWC 560), as a follow-up to coordinated multi-wavelength\n observations obtained during its recent outburst (ATel \\#8653,\n \\#8832, \\#8957; \\#10281). This system is a perfect place in\n which to study the relationship between an accretion disk and\n disk winds/jets, and a high-value target for which even low-\n resolution spectra can be extraordinarily useful...Optical\n brightening in MWC 560 tends to predict higher-velocity\n absorption, but sometimes jumps in absorption velocity also\n appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242,\n 187). If such a velocity jump occurs during photometric\n quiescence, it may prompt radio observations to confirm and test\n the proposed outflow origin for recently-discovered flat-\n spectrum radio emission (Lucy et al. ATel\n \\#10281)...Furthermore, volunteer spectroscopic monitoring of\n this system has proved useful in unpredictable ways. For\n example, \'amateur\' spectra obtained by Somogyi P{\\\'e}ter in 2015\n December demonstrated that the velocity of absorption was very\n low only a month before an optical outburst peak prompted\n absorption troughs up to 3000 km/s, which constrains very well\n the timing of the changes to the outflow to a degree that would\n not have been otherwise possible. Any resolution can be useful.\n A wavelength range that can accommodate a blueshift of at least\n 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha\n at 6562 angstroms and/or H-beta at 4861 angstroms is ideal,\n though spectra with a smaller range can still be useful.\n Photometry could potentially still be useful, but will be\n supplementary to medium-cadence photometry being collected by\n the ANS collaboration.\'\' \'\'Spectroscopy may be uploaded to the\n ARAS database\n (http://www.astrosurf.com/aras/Aras\\_DataBase/DataBase.htm), or\n sent to Adrian and Jeno directly at\n $\\lt$lucy@astro.columbia.edu$\\gt$. Finder charts with sequence\n may be created using the AAVSO Variable Star Plotter\n (https://www.aavso.org/vsp). Photometry should be submitted to\n the AAVSO International Database. See full Special Notice for\n more details. \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2017sptz.prop13168Y,\n author = {{Yan}, Lin},\n title = "{Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves}",\n howpublished = {Spitzer Proposal ID 13168},\n year = 2017,\n month = apr,\n pages = {13168},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MASTERSTHESIS{2017MsT..........2A,\n author = {{Azankpo}, Severin},\n title = "{Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope}",\n school = {University of Stellenbosch},\n year = 2017,\n month = mar,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2017MsT..........2A},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2016emo6.rept.....R,\n author = {{Rotaru}, Adrian and {Pteancu}, Mircea and {Zaharia}, Cristian},\n title = "{The penumbral Moon\'s eclipse form 16 september 2016}",\n keywords = {THE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY},\n howpublished = {http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian)},\n year = 2016,\n month = oct,\n adsurl = {https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@MISC{2016iac..talk..872V,\n author = {{Velasco}, Sergio},\n title = "{Living on the edge: Adaptive Optics+Lucky Imaging}",\n howpublished = {IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof{\\\'\\i}sica de Canarias, 872},\n year = 2016,\n month = mar,\n pages = {872},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INCOLLECTION{2009bcet.book...65L,\n author = {{Liu}, Corey W. and {Alekseyev}, Viktor Y. and {Allwardt}, Jeffrey R. and {Bankovich}, Alexander J. and {Cade-Menun}, Barbara J. and {Davis}, Ronald W. and {Du}, Lin-Shu and {Garcia}, K. Christopher and {Herschlag}, Daniel and {Khosla}, Chaitan and {Kraut}, Daniel A. and {Li}, Qing and {Null}, Brian and {Puglisi}, Joseph D. and {Sigala}, Paul A. and {Stebbins}, Jonathan F. and {Varani}, Luca},\n title = "{The Diversity of Nuclear Magnetic Resonance Spectroscopy}",\n keywords = {Physics},\n booktitle = {Biophysics and the Challenges of Emerging Threats},\n year = 2009,\n editor = {{Puglisi}, Joseph D.},\n pages = {65},\n abstract = "{The discovery of the physical phenomenon of Nuclear Magnetic Resonance\n (NMR) in 1946 gave rise to the spectroscopic technique that has\n become a remarkably versatile research tool. One could\n oversimplify NMR spectros-copy by categorizing it into the two\n broad applications of structure elucidation of molecules\n (associated with chemistry and biology) and imaging (associated\n with medicine). But, this certainly does not do NMR spectroscopy\n justice in demonstrating its general acceptance and utilization\n across the sciences. This manuscript is not an effort to present\n an exhaustive, or even partial review of NMR spectroscopy\n applications, but rather to provide a glimpse at the wide-\n ranging uses of NMR spectroscopy found within the confines of a\n single magnetic resonance research facility, the Stanford\n Magnetic Resonance Laboratory. Included here are summaries of\n projects involving protein structure determination, mapping of\n intermolecular interactions, exploring fundamental biological\n mechanisms, following compound cycling in the environmental,\n analysis of synthetic solid compounds, and microimaging of a\n model organism. \\textbackslash\\textbackslash}",\n doi = {10.1007/978-90-481-2368-1_5},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{2007AAS...210.2104M,\n author = {{Mahabal}, Ashish A. and {Drake}, A.~J. and {Djorgovski}, S.~G. and {Donalek}, C. and {Glikman}, E. and {Graham}, M.~J. and {Williams}, R. and {Baltay}, C. and {Rabinowitz}, D. and {PQ Team Caltech} and {Yale} and {NCSA} and {Indiana} and {}, . . .},\n title = "{Time Domain Exploration with the Palomar-QUEST Sky Survey}",\n booktitle = {American Astronomical Society Meeting Abstracts \\#210},\n year = 2007,\n series = {American Astronomical Society Meeting Abstracts},\n volume = {210},\n month = may,\n eid = {21.04},\n pages = {21.04},\n abstract = "{Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing\n data from driftscans in real-time. As four photometric\n bandpasses are utilized in nearly simultaneously, PQ is well\n suited to search for transient and highly variable objects.\n Using a series of software filters i.e. programs to\n select/deselect objects based on certain criteria we shorten the\n list of candidates from the initially flagged candidate\n transients. Such filters include looking for known asteroids,\n known variables, as well as moving, but previously uncatalogued\n objects based on their motion within a scan as well as between\n successive scans. Some software filters also deal with\n instrumental artifacts, edge effects, and use clustering of\n spurious detections around bright stars. During a typical night\n when we cover about 500 sq. degrees, we detect hundreds of\n asteroids, the primary contaminants in the search for\n astrophysical transients beyond our solar system.\n \\textbackslash\\textbackslashHere we describe some statistics\n based on the software filters we employ and the nature of the\n objects that seem to survive the process. We also discuss the\n usefulness of this to amateur astronomers, projects like\n VOEventNet, and other synoptic sky surveys.\n \\textbackslash\\textbackslashWe also present an outline of the\n work we have started on quantifying the variability of quasars,\n blazars, as well as various classes of Galactic sources, by\n combining the large number of PQ scans with other existing data\n sources federated in the Virtual Observatory environment.\n \\textbackslash\\textbackslashThe PQ survey is partially supported\n by the U.S. National Science Foundation (NSF).\n \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2007RJPh....1...35.,\n author = {{.}, S.~N. Agbo and {.}, E.~C. Okoroigwe},\n title = "{Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater}",\n journal = {Research Journal of Physics},\n year = 2007,\n month = jan,\n volume = {1},\n number = {1},\n pages = {35-41},\n abstract = "{Not Available \\textbackslash\\textbackslash}",\n doi = {10.3923/rjp.2007.35.41},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{1995ans..agar..390M,\n author = {{Miller}, Judy L.},\n title = "{Spacecraft navigation requirements}",\n keywords = {Earth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space Navigation, Spacecraft Trajectories, Support Systems, Technology Assessment, Technology Utilization, Ascent Trajectories, Reentry Trajectories, Spacecraft, Spacecraft Performance, Spacecraft Survivability, Tradeoffs, Weight (Mass), Space Communications, Spacecraft Communications, Command and Tracking},\n booktitle = {In AGARD},\n year = 1995,\n month = jun,\n pages = {390-405},\n abstract = "{Spacecraft operation depends upon knowledge of vehicular position and,\n consequently, navigational support has been required for all\n such systems. Technical requirements for different mission\n trajectories and orbits are addressed with consideration given\n to the various tradeoffs which may need to be considered. The\n broad spectrum of spacecraft are considered with emphasis upon\n those of greater military significance (i.e., near earth\n orbiting satellites). Technical requirements include, but are\n not limited to, accuracy; physical characteristics such as\n weight and volume; support requirements such as electrical power\n and ground support; and system integrity. Generic navigation\n suites for spacecraft applications are described. It is shown\n that operational spacecraft rely primarily upon ground-based\n tracking and computational centers with little or no\n navigational function allocated to the vehicle, while technology\n development efforts have been and continue to be directed\n primarily toward onboard navigation suites. The military\n significance of onboard navigators is shown to both improve\n spacecraft survivability and performance (accuracy).\n \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@BOOK{1995anda.book.....N,\n author = {{Nayfeh}, Ali H. and {Balachandran}, Balakumar},\n title = "{Applied nonlinear dynamics: analytical, computational and experimental methods}",\n year = 1995,\n adsurl = {https://ui.adsabs.harvard.edu/abs/1995anda.book.....N},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{1991hep.th....8028G,\n author = {{Ginsparg}, Paul},\n title = "{Applied Conformal Field Theory}",\n journal = {arXiv e-prints},\n keywords = {High Energy Physics - Theory},\n year = 1988,\n month = nov,\n eid = {hep-th/9108028},\n pages = {hep-th/9108028},\n abstract = "{These lectures consisted of an elementary introduction to conformal\n field theory, with some applications to statistical mechanical\n systems, and fewer to string theory. Contents: 1. Conformal\n theories in d dimensions 2. Conformal theories in 2 dimensions\n 3. The central charge and the Virasoro algebra 4. Kac\n determinant and unitarity 5. Identication of m = 3 with the\n critical Ising model 6. Free bosons and fermions 7. Free\n fermions on a torus 8. Free bosons on a torus 9. Affine Kac-\n Moody algebras and coset constructions 10. Advanced applications\n \\textbackslash\\textbackslash}",\narchivePrefix = {arXiv},\n eprint = {hep-th/9108028},\n primaryClass = {hep-th},\n adsurl = {https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PROCEEDINGS{1983aiaa.meetY....K,\n title = "{Autonomous navigation using lunar beacons}",\n keywords = {Artificial Satellites, Autonomous Navigation, Earth-Moon System, Lunar Communication, Radio Beacons, Radio Navigation, Space Navigation, Doppler Navigation, Least Squares Method, Orbit Calculation, Space Communications, Spacecraft Communications, Command and Tracking},\n booktitle = {AIAA, Aerospace Sciences Meeting},\n year = 1983,\n month = jan,\n abstract = "{The concept of using lunar beacon signal transmission for on-board\n navigation for earth satellites and near-earth spacecraft is\n described. The system would require powerful transmitters on the\n earth-side of the moon\'s surface and black box receivers with\n antennae and microprocessors placed on board spacecraft for\n autonomous navigation. Spacecraft navigation requires three\n position and three velocity elements to establish location\n coordinates. Two beacons could be soft-landed on the lunar\n surface at the limits of allowable separation and each would\n transmit a wide-beam signal with cones reaching GEO heights and\n be strong enough to be received by small antennae in near-earth\n orbit. The black box processor would perform on-board\n computation with one-way Doppler/range data and dynamical\n models. Alternatively, GEO satellites such as the GPS or TDRSS\n spacecraft can be used with interferometric techniques to\n provide decimeter-level accuracy for aircraft navigation.\n \\textbackslash\\textbackslash}",\n adsurl = {https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@dataset{2012ddsw.rept.....T,\n author = {{Thornton}, P.~E. and {Thornton}, M.~M. and {Mayer}, B.~W. and {Wilhelmi}, N. and {Wei}, Y. and {Devarakonda}, R. and {Cook}, R.},\n title = "{Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008}",\n howpublished = {Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)},\n year = 2012,\n month = apr,\n doi = {10.3334/ORNLDAAC/1219},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@ARTICLE{2020EPJC...80...96D,\n author = {{Dhaygude}, Akanksha and {Desai}, Shantanu},\n title = "{Generalized Lomb{\\textendash}Scargle analysis of 36Cl decay rate measurements at PTB and BNL}",\n journal = {European Physical Journal C},\n keywords = {Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Nuclear Experiment},\n year = 2020,\n month = feb,\n abstract = "{Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl\n radioactive decay data from measurements at the Physikalisch-\n Technische Bundesanstalt (PTB), in order to verify the claims by\n Sturrock and collaborators of an influence on beta-decay rates\n measured at Brookhaven National Lab (BNL) due to the rotation-\n induced modulation of the solar neutrino flux. Their analysis\n excluded any sinusoidal modulations in the frequency range from\n 0.2 to 20/year. We carry out an independent analysis of the same\n PTB and BNL data, using the generalized Lomb{\\textendash}Scargle\n periodogram to look for any statistically significant peaks in\n the range from 0 to 14 per year, and by evaluating the\n significance of every peak using multiple methods. Our results\n for the PTB data are in agreement with those by Pomme et al. For\n BNL data, we do find peaks at some of the same frequencies as\n Sturrock et al., but the significance is much lower. All our\n analysis codes and datasets have been made publicly available.}",\n doi = {10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970},\narchivePrefix = {arXiv},\n eprint = {1912.06970},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n'} data_publisher = {'msg': 'Retrieved 5 abstracts, starting with number 1.', 'export': '@software{2024zndo..10908474S,\n author = {{Schade}, Robert},\n title = "{pc2/pqdts: v2024.2}",\n year = 2024,\n month = apr,\n eid = {10.5281/zenodo.10908474},\n doi = {10.5281/zenodo.10908474},\n version = {v2024.2},\n publisher = {Zenodo},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2024zndo..10908474S},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INPROCEEDINGS{2024wsp..conf...20V,\n author = {{Vidmachenko}, A.},\n title = "{A modern view of former rivers on Mars.}",\n keywords = {Mars, riverbeds, meandering valleys, glaciers, eternal permafrost},\n booktitle = {Proceedings of the VIII International Scientific and Practical Conference. World science priorities (February 08 {\\textendash} 09},\n year = 2024,\n month = feb,\n publisher = {World of Conferences},\n pages = {20-25},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2024wsp..conf...20V},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@INCOLLECTION{2024asal.book..204V,\n author = {{Vidmachenko}, A.},\n title = "{New generation telescopes for the astronomy of the future.}",\n keywords = {new astronomical instruments, Telescopes, telescope construction, astronomical research},\n booktitle = {In book: Astronomical almanac},\n year = 2024,\n publisher = {Kyiv},\n pages = {204-209},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2024asal.book..204V},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@PROCEEDINGS{2018scrp.conf.....K,\n title = "{Science and Computing with Raspberry Pi}",\n keywords = {single board computing, astronomy, very large array, astrophysics, visualization, data science, computing, radio astronomy},\n booktitle = {Science and Computing with Raspberry Pi},\n year = 2018,\n month = jul,\n publisher = {Morgan & Claypool},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2018scrp.conf.....K},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n@BOOK{2023uwff.book.....R,\n author = {{Renwick}, J.~A.},\n title = "{Under the weather: a future forecast for New Zealand}",\n year = 2023,\n publisher = {HarperCollins},\n adsurl = {https://ui.adsabs.harvard.edu/abs/2023uwff.book.....R},\n adsnote = {Provided by the SAO/NASA Astrophysics Data System}\n}\n\n'} diff --git a/exportsrv/tests/unittests/stubdata/cslTest.py b/exportsrv/tests/unittests/stubdata/cslTest.py index 04d72c6..4519ce1 100755 --- a/exportsrv/tests/unittests/stubdata/cslTest.py +++ b/exportsrv/tests/unittests/stubdata/cslTest.py @@ -1,25 +1,25 @@ # -*- coding: utf-8 -*- -data_AASTex= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': "\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018, Weather, 73, 1, 35. doi:10.1002/wea.3072\n\\bibitem[Fal'ko \\& Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V. \\& Thomas, C.-W.\\ 2018, 2D Materials, 5, 1, 010201. doi:10.1088/2053-1583/aa9403\n\\bibitem[Parkin et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018, Spin, 8, 4, 1877001. doi:10.1142/S2010324718770015\n\\bibitem[Dessauges-Zavadsky \\& Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M. \\& Pfenniger, D.\\ 2018, Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018, 38. doi:10.1007/978-3-662-57546-8\n\\bibitem[Pustilnik et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., et al.\\ 2018, \\prl, 120, 2, 029901. doi:10.1103/PhysRevLett.120.029901\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017, Ph.D. Thesis, Leiden University. doi:10.5281/zenodo.581221\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017, AAS Nova Highlights, 2388. \n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017, Central Bureau Electronic Telegrams, 4403, 2. \n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017, Astrophysics Source Code Library. ascl:1706.009\n\\bibitem[Siltala et al.(2017)]{2017yCat.113380453S} Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017, VizieR Online Data Catalog, J/AN/338/453. \n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017, AAVSO Special Notice \\#429, 429, 1. \n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017, Spitzer Proposal, 13168. \n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017, Masters Thesis, University of Stellenbosch. \n\\bibitem[Rotaru et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016, http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian). \n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias, 872. \n\\bibitem[Liu et al.(2009)]{2009bcet.book...65L} Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009, Biophysics and the Challenges of Emerging Threats, 65. doi:10.1007/978-90-481-2368-1\\_5\n\\bibitem[Mahabal et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007, \\aas, 210, 21.04. \n\\bibitem[. \\& .(2007)]{2007RJPh....1...35.} ., S.~N.~A. \\& ., E.~C.~O.\\ 2007, Research Journal of Physics, 1, 1, 35. doi:10.3923/rjp.2007.35.41\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995, In AGARD, 390. \n\\bibitem[Nayfeh \\& Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H. \\& Balachandran, B.\\ 1995, . \n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988, , hep-th/9108028. \n\\bibitem[Khatib et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983, AIAA, Aerospace Sciences Meeting. \n\\bibitem[Thornton et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219\n"} +data_AASTex= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': "\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018, Weather, 73, 1, 35. doi:10.1002/wea.3072\n\\bibitem[Fal'ko \\& Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V. \\& Thomas, C.-W.\\ 2018, 2D Materials, 5, 1, 010201. doi:10.1088/2053-1583/aa9403\n\\bibitem[Parkin et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018, Spin, 8, 4, 1877001. doi:10.1142/S2010324718770015\n\\bibitem[Dessauges-Zavadsky \\& Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M. \\& Pfenniger, D.\\ 2018, Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018, 38. doi:10.1007/978-3-662-57546-8\n\\bibitem[Pustilnik et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., et al.\\ 2018, \\prl, 120, 2, 029901. doi:10.1103/PhysRevLett.120.029901\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017, Ph.D. Thesis, Leiden University. doi:10.5281/zenodo.581221\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017, AAS Nova Highlights, 2388. \n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017, Central Bureau Electronic Telegrams, 4403, 2. \n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017, Astrophysics Source Code Library. ascl:1706.009\n\\bibitem[Siltala et al.(2017)]{2017yCat.113380453S} Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017, VizieR Online Data Catalog, J/AN/338/453. \n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017, AAVSO Special Notice \\#429, 429, 1. \n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017, Spitzer Proposal, 13168. \n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017, Masters Thesis, University of Stellenbosch. \n\\bibitem[Rotaru et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016, http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian). \n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias, 872. \n\\bibitem[Liu et al.(2009)]{2009bcet.book...65L} Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009, Biophysics and the Challenges of Emerging Threats, 65. doi:10.1007/978-90-481-2368-1\\_5\n\\bibitem[Mahabal et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007, \\aas, 210, 21.04. \n\\bibitem[. \\& .(2007)]{2007RJPh....1...35.} ., S.~N.~A. \\& ., E.~C.~O.\\ 2007, Research Journal of Physics, 1, 1, 35. doi:10.3923/rjp.2007.35.41\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995, In AGARD, 390. \n\\bibitem[Nayfeh \\& Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H. \\& Balachandran, B.\\ 1995, . \n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988, , hep-th/9108028. \n\\bibitem[Khatib et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983, AIAA, Aerospace Sciences Meeting. \n\\bibitem[Thornton et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219\n\\bibitem[Dhaygude \\& Desai(2020)]{2020EPJC...80...96D} Dhaygude, A. \\& Desai, S.\\ 2020, European Physical Journal C. doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\n"} -data_AASTex_PSJ= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': "\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018, Weather, Book reviews, 73, 1, 35. doi:10.1002/wea.3072\n\\bibitem[Fal'ko \\& Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V. \\& Thomas, C.-W.\\ 2018, 2D Materials, 2D Materials: maintaining editorial quality, 5, 1, 010201. doi:10.1088/2053-1583/aa9403\n\\bibitem[Parkin et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018, Spin, Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor, 8, 4, 1877001. doi:10.1142/S2010324718770015\n\\bibitem[Dessauges-Zavadsky \\& Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M. \\& Pfenniger, D.\\ 2018, Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018, Millimeter Astronomy, 38. doi:10.1007/978-3-662-57546-8\n\\bibitem[Pustilnik et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., et al.\\ 2018, \\prl, Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)], 120, 2, 029901. doi:10.1103/PhysRevLett.120.029901\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017, Ph.D. Thesis, Resolving Gas-Phase Metallicity In Galaxies, Leiden University. doi:10.5281/zenodo.581221\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017, AAS Nova Highlights, A 3D View of a Supernova Remnant, 2388. \n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017, Central Bureau Electronic Telegrams, Potential New Meteor Shower from Comet C/2015 D4 (Borisov), 4403, 2. \n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017, Astrophysics Source Code Library, sick: Spectroscopic inference crank. ascl:1706.009\n\\bibitem[Siltala et al.(2017)]{2017yCat.113380453S} Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017, VizieR Online Data Catalog, VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017), J/AN/338/453. \n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017, AAVSO Special Notice \\#429, V694 Mon (MWC 560) spectroscopy requested, 429, 1. \n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017, Spitzer Proposal, Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves, 13168. \n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017, Masters Thesis, Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope, University of Stellenbosch. \n\\bibitem[Rotaru et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016, http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian), The penumbral Moon's eclipse form 16 september 2016. \n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias, Living on the edge: Adaptive Optics+Lucky Imaging, 872. \n\\bibitem[Liu et al.(2009)]{2009bcet.book...65L} Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009, Biophysics and the Challenges of Emerging Threats, The Diversity of Nuclear Magnetic Resonance Spectroscopy, 65. doi:10.1007/978-90-481-2368-1\\_5\n\\bibitem[Mahabal et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007, \\aas, Time Domain Exploration with the Palomar-QUEST Sky Survey, 210, 21.04. \n\\bibitem[. \\& .(2007)]{2007RJPh....1...35.} ., S.~N.~A. \\& ., E.~C.~O.\\ 2007, Research Journal of Physics, Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater, 1, 1, 35. doi:10.3923/rjp.2007.35.41\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995, In AGARD, Spacecraft navigation requirements, 390. \n\\bibitem[Nayfeh \\& Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H. \\& Balachandran, B.\\ 1995, , Applied nonlinear dynamics: analytical, computational and experimental methods. \n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988, , Applied Conformal Field Theory, hep-th/9108028. \n\\bibitem[Khatib et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983, AIAA, Aerospace Sciences Meeting, Autonomous navigation using lunar beacons. \n\\bibitem[Thornton et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC, Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008. doi:10.3334/ORNLDAAC/1219\n"} +data_AASTex_PSJ= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': "\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018, Weather, Book reviews, 73, 1, 35. doi:10.1002/wea.3072\n\\bibitem[Fal'ko \\& Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V. \\& Thomas, C.-W.\\ 2018, 2D Materials, 2D Materials: maintaining editorial quality, 5, 1, 010201. doi:10.1088/2053-1583/aa9403\n\\bibitem[Parkin et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018, Spin, Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor, 8, 4, 1877001. doi:10.1142/S2010324718770015\n\\bibitem[Dessauges-Zavadsky \\& Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M. \\& Pfenniger, D.\\ 2018, Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018, Millimeter Astronomy, 38. doi:10.1007/978-3-662-57546-8\n\\bibitem[Pustilnik et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., et al.\\ 2018, \\prl, Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)], 120, 2, 029901. doi:10.1103/PhysRevLett.120.029901\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017, Ph.D. Thesis, Resolving Gas-Phase Metallicity In Galaxies, Leiden University. doi:10.5281/zenodo.581221\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017, AAS Nova Highlights, A 3D View of a Supernova Remnant, 2388. \n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017, Central Bureau Electronic Telegrams, Potential New Meteor Shower from Comet C/2015 D4 (Borisov), 4403, 2. \n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017, Astrophysics Source Code Library, sick: Spectroscopic inference crank. ascl:1706.009\n\\bibitem[Siltala et al.(2017)]{2017yCat.113380453S} Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017, VizieR Online Data Catalog, VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017), J/AN/338/453. \n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017, AAVSO Special Notice \\#429, V694 Mon (MWC 560) spectroscopy requested, 429, 1. \n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017, Spitzer Proposal, Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves, 13168. \n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017, Masters Thesis, Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope, University of Stellenbosch. \n\\bibitem[Rotaru et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016, http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian), The penumbral Moon's eclipse form 16 september 2016. \n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias, Living on the edge: Adaptive Optics+Lucky Imaging, 872. \n\\bibitem[Liu et al.(2009)]{2009bcet.book...65L} Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009, Biophysics and the Challenges of Emerging Threats, The Diversity of Nuclear Magnetic Resonance Spectroscopy, 65. doi:10.1007/978-90-481-2368-1\\_5\n\\bibitem[Mahabal et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007, \\aas, Time Domain Exploration with the Palomar-QUEST Sky Survey, 210, 21.04. \n\\bibitem[. \\& .(2007)]{2007RJPh....1...35.} ., S.~N.~A. \\& ., E.~C.~O.\\ 2007, Research Journal of Physics, Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater, 1, 1, 35. doi:10.3923/rjp.2007.35.41\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995, In AGARD, Spacecraft navigation requirements, 390. \n\\bibitem[Nayfeh \\& Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H. \\& Balachandran, B.\\ 1995, , Applied nonlinear dynamics: analytical, computational and experimental methods. \n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988, , Applied Conformal Field Theory, hep-th/9108028. \n\\bibitem[Khatib et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983, AIAA, Aerospace Sciences Meeting, Autonomous navigation using lunar beacons. \n\\bibitem[Thornton et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC, Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008. doi:10.3334/ORNLDAAC/1219\n\\bibitem[Dhaygude \\& Desai(2020)]{2020EPJC...80...96D} Dhaygude, A. \\& Desai, S.\\ 2020, European Physical Journal C, Generalized Lomb{\\textendash}Scargle analysis of 36Cl decay rate measurements at PTB and BNL. doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\n"} -data_Icarus= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': u"\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018.\\ Book reviews.\\ Weather 73, 35–35. doi:10.1002/wea.3072\n\\bibitem[Fal'ko and Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V., Thomas, C.-W.\\ 2018.\\ 2D Materials: maintaining editorial quality.\\ 2D Materials 5. doi:10.1088/2053-1583/aa9403\n\\bibitem[Parkin et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., Chang, C.-R.\\ 2018.\\ Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor.\\ Spin 8. doi:10.1142/S2010324718770015\n\\bibitem[Dessauges-Zavadsky and Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M., Pfenniger, D.\\ 2018.\\ Millimeter Astronomy.\\ Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018 38. doi:10.1007/978-3-662-57546-8\n\\bibitem[Pustilnik et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., Glazman, L.~I.\\ 2018.\\ Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)].\\ Physical Review Letters 120. doi:10.1103/PhysRevLett.120.029901\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017.\\ Resolving Gas-Phase Metallicity In Galaxies.\\ Ph.D. Thesis. doi:10.5281/zenodo.581221\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017.\\ A 3D View of a Supernova Remnant.\\ AAS Nova Highlights.\n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017.\\ Potential New Meteor Shower from Comet C/2015 D4 (Borisov).\\ Central Bureau Electronic Telegrams 4403.\n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017.\\ sick: Spectroscopic inference crank.\\ Astrophysics Source Code Library. ascl:1706.009\n\\bibitem[Siltala et al.(2017)]{2017yCat.113380453S} Siltala, J. and 12 colleagues 2017.\\ VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017).\\ VizieR Online Data Catalog.\n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017.\\ V694 Mon (MWC 560) spectroscopy requested.\\ AAVSO Special Notice \\#429 429.\n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017.\\ Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves.\\ Spitzer Proposal, 13168.\n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017.\\ Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope.\\ Masters Thesis, 2.\n\\bibitem[Rotaru et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., Zaharia, C.\\ 2016.\\ The penumbral Moon's eclipse form 16 september 2016.\\ http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian).\n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016.\\ Living on the edge: Adaptive Optics+Lucky Imaging.\\ IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias.\n\\bibitem[Liu et al.(2009)]{2009bcet.book...65L} Liu, C.~W. and 16 colleagues 2009.\\ The Diversity of Nuclear Magnetic Resonance Spectroscopy.\\ Biophysics and the Challenges of Emerging Threats 65. doi:10.1007/978-90-481-2368-1\\_5\n\\bibitem[Mahabal et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A. and 13 colleagues 2007.\\ Time Domain Exploration with the Palomar-QUEST Sky Survey.\\ American Astronomical Society Meeting Abstracts \\#210.\n\\bibitem[. and .(2007)]{2007RJPh....1...35.} ., S.~N.~A., ., E.~C.~O.\\ 2007.\\ Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater.\\ Research Journal of Physics 1, 35–41. doi:10.3923/rjp.2007.35.41\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995.\\ Spacecraft navigation requirements.\\ In AGARD, 390–405.\n\\bibitem[Nayfeh and Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H., Balachandran, B.\\ 1995.\\ Applied nonlinear dynamics: analytical, computational and experimental methods.\\ Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995.\n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988.\\ Applied Conformal Field Theory.\\ arXiv e-prints.\n\\bibitem[Khatib et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., Null, G., Yunck, T., Wu, S.\\ 1983.\\ Autonomous navigation using lunar beacons.\\ AIAA, Aerospace Sciences Meeting.\n\\bibitem[Thornton et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E. and 6 colleagues 2012.\\ Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008.\\ Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219\n"} +data_Icarus= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': u"\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018.\\ Book reviews.\\ Weather 73, 35–35. doi:10.1002/wea.3072\n\\bibitem[Fal'ko and Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V., Thomas, C.-W.\\ 2018.\\ 2D Materials: maintaining editorial quality.\\ 2D Materials 5. doi:10.1088/2053-1583/aa9403\n\\bibitem[Parkin et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., Chang, C.-R.\\ 2018.\\ Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor.\\ Spin 8. doi:10.1142/S2010324718770015\n\\bibitem[Dessauges-Zavadsky and Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M., Pfenniger, D.\\ 2018.\\ Millimeter Astronomy.\\ Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018 38. doi:10.1007/978-3-662-57546-8\n\\bibitem[Pustilnik et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., Glazman, L.~I.\\ 2018.\\ Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)].\\ Physical Review Letters 120. doi:10.1103/PhysRevLett.120.029901\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017.\\ Resolving Gas-Phase Metallicity In Galaxies.\\ Ph.D. Thesis. doi:10.5281/zenodo.581221\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017.\\ A 3D View of a Supernova Remnant.\\ AAS Nova Highlights.\n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017.\\ Potential New Meteor Shower from Comet C/2015 D4 (Borisov).\\ Central Bureau Electronic Telegrams 4403.\n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017.\\ sick: Spectroscopic inference crank.\\ Astrophysics Source Code Library. ascl:1706.009\n\\bibitem[Siltala et al.(2017)]{2017yCat.113380453S} Siltala, J. and 12 colleagues 2017.\\ VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017).\\ VizieR Online Data Catalog.\n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017.\\ V694 Mon (MWC 560) spectroscopy requested.\\ AAVSO Special Notice \\#429 429.\n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017.\\ Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves.\\ Spitzer Proposal, 13168.\n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017.\\ Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope.\\ Masters Thesis, 2.\n\\bibitem[Rotaru et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., Zaharia, C.\\ 2016.\\ The penumbral Moon's eclipse form 16 september 2016.\\ http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian).\n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016.\\ Living on the edge: Adaptive Optics+Lucky Imaging.\\ IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias.\n\\bibitem[Liu et al.(2009)]{2009bcet.book...65L} Liu, C.~W. and 16 colleagues 2009.\\ The Diversity of Nuclear Magnetic Resonance Spectroscopy.\\ Biophysics and the Challenges of Emerging Threats 65. doi:10.1007/978-90-481-2368-1\\_5\n\\bibitem[Mahabal et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A. and 13 colleagues 2007.\\ Time Domain Exploration with the Palomar-QUEST Sky Survey.\\ American Astronomical Society Meeting Abstracts \\#210.\n\\bibitem[. and .(2007)]{2007RJPh....1...35.} ., S.~N.~A., ., E.~C.~O.\\ 2007.\\ Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater.\\ Research Journal of Physics 1, 35–41. doi:10.3923/rjp.2007.35.41\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995.\\ Spacecraft navigation requirements.\\ In AGARD, 390–405.\n\\bibitem[Nayfeh and Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H., Balachandran, B.\\ 1995.\\ Applied nonlinear dynamics: analytical, computational and experimental methods.\\ Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995.\n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988.\\ Applied Conformal Field Theory.\\ arXiv e-prints.\n\\bibitem[Khatib et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., Null, G., Yunck, T., Wu, S.\\ 1983.\\ Autonomous navigation using lunar beacons.\\ AIAA, Aerospace Sciences Meeting.\n\\bibitem[Thornton et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E. and 6 colleagues 2012.\\ Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008.\\ Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219\n\\bibitem[Dhaygude and Desai(2020)]{2020EPJC...80...96D} Dhaygude, A., Desai, S.\\ 2020.\\ Generalized Lomb{\\textendash}Scargle analysis of 36Cl decay rate measurements at PTB and BNL.\\ European Physical Journal C. doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\n"} -data_MNRAS = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': "\\bibitem[\\protect\\citeauthoryear{No author}{2018}]{2018Wthr...73Q..35.} No author, 2018, Wthr, 73, 35. doi:10.1002/wea.3072\n\\bibitem[\\protect\\citeauthoryear{Fal'ko \\& Thomas}{2018}]{2018TDM.....5a0201F} Fal'ko V., Thomas C.-W., 2018, TDM, 5, 010201. doi:10.1088/2053-1583/aa9403\n\\bibitem[\\protect\\citeauthoryear{Parkin, Chantrell, \\& Chang}{2018}]{2018Spin....877001P} Parkin S., Chantrell R., Chang C.-R., 2018, Spin, 8, 1877001. doi:10.1142/S2010324718770015\n\\bibitem[\\protect\\citeauthoryear{Dessauges-Zavadsky \\& Pfenniger}{2018}]{2018SAAS...38.....D} Dessauges-Zavadsky M., Pfenniger D., 2018, SAAS, 38. doi:10.1007/978-3-662-57546-8\n\\bibitem[\\protect\\citeauthoryear{Pustilnik et al.}{2018}]{2018PhRvL.120b9901P} Pustilnik M., van Heck B., Lutchyn R.~M., Glazman L.~I., 2018, PhRvL, 120, 029901. doi:10.1103/PhysRevLett.120.029901\n\\bibitem[\\protect\\citeauthoryear{Carton}{2017}]{2017PhDT........14C} Carton D., 2017, PhDT. doi:10.5281/zenodo.581221\n\\bibitem[\\protect\\citeauthoryear{Kohler}{2017}]{2017nova.pres.2388K} Kohler S., 2017, nova.pres, 2388\n\\bibitem[\\protect\\citeauthoryear{Green}{2017}]{2017CBET.4403....2G} Green D.~W.~E., 2017, CBET, 4403, 2\n\\bibitem[\\protect\\citeauthoryear{Casey}{2017}]{2017ascl.soft06009C} Casey A.~R., 2017, ascl.soft. ascl:1706.009\n\\bibitem[\\protect\\citeauthoryear{Siltala et al.}{2017}]{2017yCat.113380453S} Siltala J., Jetsu L., Hackman T., Henry G.~W., Immonen L., Kajatkari P., Lankinen J., et al., 2017, yCat, J/AN/338/453\n\\bibitem[\\protect\\citeauthoryear{Waagen}{2017}]{2017AAVSN.429....1W} Waagen E.~O., 2017, AAVSN, 429, 1\n\\bibitem[\\protect\\citeauthoryear{Yan}{2017}]{2017sptz.prop13168Y} Yan L., 2017, sptz.prop, 13168\n\\bibitem[\\protect\\citeauthoryear{Azankpo}{2017}]{2017MsT..........2A} Azankpo S., 2017, MsT, 2\n\\bibitem[\\protect\\citeauthoryear{Rotaru, Pteancu, \\& Zaharia}{2016}]{2016emo6.rept.....R} Rotaru A., Pteancu M., Zaharia C., 2016, emo6.rept\n\\bibitem[\\protect\\citeauthoryear{Velasco}{2016}]{2016iac..talk..872V} Velasco S., 2016, iac..talk, 872\n\\bibitem[\\protect\\citeauthoryear{Liu et al.}{2009}]{2009bcet.book...65L} Liu C.~W., Alekseyev V.~Y., Allwardt J.~R., Bankovich A.~J., Cade-Menun B.~J., Davis R.~W., Du L.-S., et al., 2009, bcet.book, 65. doi:10.1007/978-90-481-2368-1\\_5\n\\bibitem[\\protect\\citeauthoryear{Mahabal et al.}{2007}]{2007AAS...210.2104M} Mahabal A.~A., Drake A.~J., Djorgovski S.~G., Donalek C., Glikman E., Graham M.~J., Williams R., et al., 2007, AAS, 210, 21.04\n\\bibitem[\\protect\\citeauthoryear{. \\& .}{2007}]{2007RJPh....1...35.} . S.~N.~A., . E.~C.~O., 2007, RJPh, 1, 35. doi:10.3923/rjp.2007.35.41\n\\bibitem[\\protect\\citeauthoryear{Miller}{1995}]{1995ans..agar..390M} Miller J.~L., 1995, ans..agar, 390\n\\bibitem[\\protect\\citeauthoryear{Nayfeh \\& Balachandran}{1995}]{1995anda.book.....N} Nayfeh A.~H., Balachandran B., 1995, anda.book\n\\bibitem[\\protect\\citeauthoryear{Ginsparg}{1988}]{1991hep.th....8028G} Ginsparg P., 1988, arXiv, hep-th/9108028\n\\bibitem[\\protect\\citeauthoryear{Khatib et al.}{1983}]{1983aiaa.meetY....K} Khatib A.~R., Ellis J., French J., Null G., Yunck T., Wu S., 1983, aiaa.meet\n\\bibitem[\\protect\\citeauthoryear{Thornton et al.}{2012}]{2012ddsw.rept.....T} Thornton P.~E., Thornton M.~M., Mayer B.~W., Wilhelmi N., Wei Y., Devarakonda R., Cook R., 2012, ddsw.rept. doi:10.3334/ORNLDAAC/1219\n"} +data_MNRAS = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': "\\bibitem[\\protect\\citeauthoryear{No author}{2018}]{2018Wthr...73Q..35.} No author, 2018, Wthr, 73, 35. doi:10.1002/wea.3072\n\\bibitem[\\protect\\citeauthoryear{Fal'ko \\& Thomas}{2018}]{2018TDM.....5a0201F} Fal'ko V., Thomas C.-W., 2018, TDM, 5, 010201. doi:10.1088/2053-1583/aa9403\n\\bibitem[\\protect\\citeauthoryear{Parkin, Chantrell, \\& Chang}{2018}]{2018Spin....877001P} Parkin S., Chantrell R., Chang C.-R., 2018, Spin, 8, 1877001. doi:10.1142/S2010324718770015\n\\bibitem[\\protect\\citeauthoryear{Dessauges-Zavadsky \\& Pfenniger}{2018}]{2018SAAS...38.....D} Dessauges-Zavadsky M., Pfenniger D., 2018, SAAS, 38. doi:10.1007/978-3-662-57546-8\n\\bibitem[\\protect\\citeauthoryear{Pustilnik et al.}{2018}]{2018PhRvL.120b9901P} Pustilnik M., van Heck B., Lutchyn R.~M., Glazman L.~I., 2018, PhRvL, 120, 029901. doi:10.1103/PhysRevLett.120.029901\n\\bibitem[\\protect\\citeauthoryear{Carton}{2017}]{2017PhDT........14C} Carton D., 2017, PhDT. doi:10.5281/zenodo.581221\n\\bibitem[\\protect\\citeauthoryear{Kohler}{2017}]{2017nova.pres.2388K} Kohler S., 2017, nova.pres, 2388\n\\bibitem[\\protect\\citeauthoryear{Green}{2017}]{2017CBET.4403....2G} Green D.~W.~E., 2017, CBET, 4403, 2\n\\bibitem[\\protect\\citeauthoryear{Casey}{2017}]{2017ascl.soft06009C} Casey A.~R., 2017, ascl.soft. ascl:1706.009\n\\bibitem[\\protect\\citeauthoryear{Siltala et al.}{2017}]{2017yCat.113380453S} Siltala J., Jetsu L., Hackman T., Henry G.~W., Immonen L., Kajatkari P., Lankinen J., et al., 2017, yCat, J/AN/338/453\n\\bibitem[\\protect\\citeauthoryear{Waagen}{2017}]{2017AAVSN.429....1W} Waagen E.~O., 2017, AAVSN, 429, 1\n\\bibitem[\\protect\\citeauthoryear{Yan}{2017}]{2017sptz.prop13168Y} Yan L., 2017, sptz.prop, 13168\n\\bibitem[\\protect\\citeauthoryear{Azankpo}{2017}]{2017MsT..........2A} Azankpo S., 2017, MsT, 2\n\\bibitem[\\protect\\citeauthoryear{Rotaru, Pteancu, \\& Zaharia}{2016}]{2016emo6.rept.....R} Rotaru A., Pteancu M., Zaharia C., 2016, emo6.rept\n\\bibitem[\\protect\\citeauthoryear{Velasco}{2016}]{2016iac..talk..872V} Velasco S., 2016, iac..talk, 872\n\\bibitem[\\protect\\citeauthoryear{Liu et al.}{2009}]{2009bcet.book...65L} Liu C.~W., Alekseyev V.~Y., Allwardt J.~R., Bankovich A.~J., Cade-Menun B.~J., Davis R.~W., Du L.-S., et al., 2009, bcet.book, 65. doi:10.1007/978-90-481-2368-1\\_5\n\\bibitem[\\protect\\citeauthoryear{Mahabal et al.}{2007}]{2007AAS...210.2104M} Mahabal A.~A., Drake A.~J., Djorgovski S.~G., Donalek C., Glikman E., Graham M.~J., Williams R., et al., 2007, AAS, 210, 21.04\n\\bibitem[\\protect\\citeauthoryear{. \\& .}{2007}]{2007RJPh....1...35.} . S.~N.~A., . E.~C.~O., 2007, RJPh, 1, 35. doi:10.3923/rjp.2007.35.41\n\\bibitem[\\protect\\citeauthoryear{Miller}{1995}]{1995ans..agar..390M} Miller J.~L., 1995, ans..agar, 390\n\\bibitem[\\protect\\citeauthoryear{Nayfeh \\& Balachandran}{1995}]{1995anda.book.....N} Nayfeh A.~H., Balachandran B., 1995, anda.book\n\\bibitem[\\protect\\citeauthoryear{Ginsparg}{1988}]{1991hep.th....8028G} Ginsparg P., 1988, arXiv, hep-th/9108028\n\\bibitem[\\protect\\citeauthoryear{Khatib et al.}{1983}]{1983aiaa.meetY....K} Khatib A.~R., Ellis J., French J., Null G., Yunck T., Wu S., 1983, aiaa.meet\n\\bibitem[\\protect\\citeauthoryear{Thornton et al.}{2012}]{2012ddsw.rept.....T} Thornton P.~E., Thornton M.~M., Mayer B.~W., Wilhelmi N., Wei Y., Devarakonda R., Cook R., 2012, ddsw.rept. doi:10.3334/ORNLDAAC/1219\n\\bibitem[\\protect\\citeauthoryear{Dhaygude \\& Desai}{2020}]{2020EPJC...80...96D} Dhaygude A., Desai S., 2020, EPJC. doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\n"} -data_SoPh= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': "\\bibitem[No author(2018)]{2018Wthr...73Q..35.}No author: 2018, {\\it Weather} {\\bf 73}, 35. doi:10.1002/wea.3072.\n\\bibitem[Fal'ko and Thomas(2018)]{2018TDM.....5a0201F}Fal'ko, V. and Thomas, C.-W.: 2018, {\\it 2D Materials} {\\bf 5}, 010201. doi:10.1088/2053-1583/aa9403.\n\\bibitem[Parkin, Chantrell, and Chang(2018)]{2018Spin....877001P}Parkin, S., Chantrell, R., and Chang, C.-R.: 2018, {\\it Spin} {\\bf 8}, 1877001. doi:10.1142/S2010324718770015.\n\\bibitem[Dessauges-Zavadsky and Pfenniger(2018)]{2018SAAS...38.....D}Dessauges-Zavadsky, M. and Pfenniger, D.: 2018, {\\it Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018} {\\bf 38}. doi:10.1007/978-3-662-57546-8.\n\\bibitem[Pustilnik \\emph{et al.}(2018)]{2018PhRvL.120b9901P}Pustilnik, M., van Heck, B., Lutchyn, R.M., and Glazman, L.I.: 2018, {\\it Physical Review Letters} {\\bf 120}, 029901. doi:10.1103/PhysRevLett.120.029901.\n\\bibitem[Carton(2017)]{2017PhDT........14C}Carton, D.: 2017, {\\it Ph.D. Thesis}. doi:10.5281/zenodo.581221.\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K}Kohler, S.: 2017, {\\it AAS Nova Highlights}, 2388.\n\\bibitem[Green(2017)]{2017CBET.4403....2G}Green, D.W.E.: 2017, {\\it Central Bureau Electronic Telegrams} {\\bf 4403}.\n\\bibitem[Casey(2017)]{2017ascl.soft06009C}Casey, A.R.: 2017, {\\it Astrophysics Source Code Library}. ascl:1706.009.\n\\bibitem[Siltala \\emph{et al.}(2017)]{2017yCat.113380453S}Siltala, J., Jetsu, L., Hackman, T., Henry, G.W., Immonen, L., Kajatkari, P., and, ...: 2017, {\\it VizieR Online Data Catalog}, J/AN/338/453.\n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W}Waagen, E.O.: 2017, {\\it AAVSO Special Notice \\#429} {\\bf 429}.\n\\bibitem[Yan(2017)]{2017sptz.prop13168Y}Yan, L.: 2017, {\\it Spitzer Proposal}, 13168.\n\\bibitem[Azankpo(2017)]{2017MsT..........2A}Azankpo, S.: 2017, {\\it Masters Thesis}, 2.\n\\bibitem[Rotaru, Pteancu, and Zaharia(2016)]{2016emo6.rept.....R}Rotaru, A., Pteancu, M., and Zaharia, C.: 2016, {\\it http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian)}.\n\\bibitem[Velasco(2016)]{2016iac..talk..872V}Velasco, S.: 2016, {\\it IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias}.\n\\bibitem[Liu \\emph{et al.}(2009)]{2009bcet.book...65L}Liu, C.W., Alekseyev, V.Y., Allwardt, J.R., Bankovich, A.J., Cade-Menun, B.J., Davis, R.W., and, ...: 2009, {\\it Biophysics and the Challenges of Emerging Threats}, 65. doi:10.1007/978-90-481-2368-1\\_5.\n\\bibitem[Mahabal \\emph{et al.}(2007)]{2007AAS...210.2104M}Mahabal, A.A., Drake, A.J., Djorgovski, S.G., Donalek, C., Glikman, E., Graham, M.J., and, ...: 2007, {\\it American Astronomical Society Meeting Abstracts \\#210} {\\bf 210}, 21.04.\n\\bibitem[. and .(2007)]{2007RJPh....1...35.}., S.N.A. and ., E.C.O.: 2007, {\\it Research Journal of Physics} {\\bf 1}, 35. doi:10.3923/rjp.2007.35.41.\n\\bibitem[Miller(1995)]{1995ans..agar..390M}Miller, J.L.: 1995, {\\it In AGARD}, 390.\n\\bibitem[Nayfeh and Balachandran(1995)]{1995anda.book.....N}Nayfeh, A.H. and Balachandran, B.: 1995, {\\it Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995}.\n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G}Ginsparg, P.: 1988, {\\it arXiv e-prints}, hep-th/9108028.\n\\bibitem[Khatib \\emph{et al.}(1983)]{1983aiaa.meetY....K}Khatib, A.R., Ellis, J., French, J., Null, G., Yunck, T., and Wu, S.: 1983, {\\it AIAA, Aerospace Sciences Meeting}.\n\\bibitem[Thornton \\emph{et al.}(2012)]{2012ddsw.rept.....T}Thornton, P.E., Thornton, M.M., Mayer, B.W., Wilhelmi, N., Wei, Y., Devarakonda, R., and, ...: 2012, {\\it Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC}. doi:10.3334/ORNLDAAC/1219.\n"} +data_SoPh= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': "\\bibitem[No author(2018)]{2018Wthr...73Q..35.}No author: 2018, {\\it Weather} {\\bf 73}, 35. doi:10.1002/wea.3072.\n\\bibitem[Fal'ko and Thomas(2018)]{2018TDM.....5a0201F}Fal'ko, V. and Thomas, C.-W.: 2018, {\\it 2D Materials} {\\bf 5}, 010201. doi:10.1088/2053-1583/aa9403.\n\\bibitem[Parkin, Chantrell, and Chang(2018)]{2018Spin....877001P}Parkin, S., Chantrell, R., and Chang, C.-R.: 2018, {\\it Spin} {\\bf 8}, 1877001. doi:10.1142/S2010324718770015.\n\\bibitem[Dessauges-Zavadsky and Pfenniger(2018)]{2018SAAS...38.....D}Dessauges-Zavadsky, M. and Pfenniger, D.: 2018, {\\it Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018} {\\bf 38}. doi:10.1007/978-3-662-57546-8.\n\\bibitem[Pustilnik \\emph{et al.}(2018)]{2018PhRvL.120b9901P}Pustilnik, M., van Heck, B., Lutchyn, R.M., and Glazman, L.I.: 2018, {\\it Physical Review Letters} {\\bf 120}, 029901. doi:10.1103/PhysRevLett.120.029901.\n\\bibitem[Carton(2017)]{2017PhDT........14C}Carton, D.: 2017, {\\it Ph.D. Thesis}. doi:10.5281/zenodo.581221.\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K}Kohler, S.: 2017, {\\it AAS Nova Highlights}, 2388.\n\\bibitem[Green(2017)]{2017CBET.4403....2G}Green, D.W.E.: 2017, {\\it Central Bureau Electronic Telegrams} {\\bf 4403}.\n\\bibitem[Casey(2017)]{2017ascl.soft06009C}Casey, A.R.: 2017, {\\it Astrophysics Source Code Library}. ascl:1706.009.\n\\bibitem[Siltala \\emph{et al.}(2017)]{2017yCat.113380453S}Siltala, J., Jetsu, L., Hackman, T., Henry, G.W., Immonen, L., Kajatkari, P., and, ...: 2017, {\\it VizieR Online Data Catalog}, J/AN/338/453.\n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W}Waagen, E.O.: 2017, {\\it AAVSO Special Notice \\#429} {\\bf 429}.\n\\bibitem[Yan(2017)]{2017sptz.prop13168Y}Yan, L.: 2017, {\\it Spitzer Proposal}, 13168.\n\\bibitem[Azankpo(2017)]{2017MsT..........2A}Azankpo, S.: 2017, {\\it Masters Thesis}, 2.\n\\bibitem[Rotaru, Pteancu, and Zaharia(2016)]{2016emo6.rept.....R}Rotaru, A., Pteancu, M., and Zaharia, C.: 2016, {\\it http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian)}.\n\\bibitem[Velasco(2016)]{2016iac..talk..872V}Velasco, S.: 2016, {\\it IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias}.\n\\bibitem[Liu \\emph{et al.}(2009)]{2009bcet.book...65L}Liu, C.W., Alekseyev, V.Y., Allwardt, J.R., Bankovich, A.J., Cade-Menun, B.J., Davis, R.W., and, ...: 2009, {\\it Biophysics and the Challenges of Emerging Threats}, 65. doi:10.1007/978-90-481-2368-1\\_5.\n\\bibitem[Mahabal \\emph{et al.}(2007)]{2007AAS...210.2104M}Mahabal, A.A., Drake, A.J., Djorgovski, S.G., Donalek, C., Glikman, E., Graham, M.J., and, ...: 2007, {\\it American Astronomical Society Meeting Abstracts \\#210} {\\bf 210}, 21.04.\n\\bibitem[. and .(2007)]{2007RJPh....1...35.}., S.N.A. and ., E.C.O.: 2007, {\\it Research Journal of Physics} {\\bf 1}, 35. doi:10.3923/rjp.2007.35.41.\n\\bibitem[Miller(1995)]{1995ans..agar..390M}Miller, J.L.: 1995, {\\it In AGARD}, 390.\n\\bibitem[Nayfeh and Balachandran(1995)]{1995anda.book.....N}Nayfeh, A.H. and Balachandran, B.: 1995, {\\it Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995}.\n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G}Ginsparg, P.: 1988, {\\it arXiv e-prints}, hep-th/9108028.\n\\bibitem[Khatib \\emph{et al.}(1983)]{1983aiaa.meetY....K}Khatib, A.R., Ellis, J., French, J., Null, G., Yunck, T., and Wu, S.: 1983, {\\it AIAA, Aerospace Sciences Meeting}.\n\\bibitem[Thornton \\emph{et al.}(2012)]{2012ddsw.rept.....T}Thornton, P.E., Thornton, M.M., Mayer, B.W., Wilhelmi, N., Wei, Y., Devarakonda, R., and, ...: 2012, {\\it Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC}. doi:10.3334/ORNLDAAC/1219.\n\\bibitem[Dhaygude and Desai(2020)]{2020EPJC...80...96D}Dhaygude, A. and Desai, S.: 2020, {\\it European Physical Journal C}. doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970.\n"} -data_ASPC= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': "\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018, Weather, 73, 35. doi:10.1002/wea.3072.\n\\bibitem[Fal'ko \\& Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V., \\& Thomas, C.-W.\\ 2018, 2D Materials, 5, 010201. doi:10.1088/2053-1583/aa9403.\n\\bibitem[Parkin, et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018, Spin, 8, 1877001. doi:10.1142/S2010324718770015.\n\\bibitem[Dessauges-Zavadsky \\& Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M., \\& Pfenniger, D.\\ 2018, Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018, 38. doi:10.1007/978-3-662-57546-8.\n\\bibitem[Pustilnik, et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., et al.\\ 2018, \\prl, 120, 029901. doi:10.1103/PhysRevLett.120.029901.\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017, Ph.D. Thesis. doi:10.5281/zenodo.581221.\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017, AAS Nova Highlights, 2388.\n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017, Central Bureau Electronic Telegrams, 4403.\n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017, Astrophysics Source Code Library. ascl:1706.009.\n\\bibitem[Siltala, et al.(2017)]{2017yCat.113380453S} Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017, VizieR Online Data Catalog, J/AN/338/453.\n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017, AAVSO Special Notice \\#429, 429.\n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017, Spitzer Proposal, 13168.\n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017, Masters Thesis, 2.\n\\bibitem[Rotaru, et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016, http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian).\n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias.\n\\bibitem[Liu, et al.(2009)]{2009bcet.book...65L} Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009, Biophysics and the Challenges of Emerging Threats, 65. doi:10.1007/978-90-481-2368-1\\_5.\n\\bibitem[Mahabal, et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007, \\aas, 210, 21.04.\n\\bibitem[. \\& .(2007)]{2007RJPh....1...35.} ., S.~N.~A., \\& ., E.~C.~O.\\ 2007, Research Journal of Physics, 1, 35. doi:10.3923/rjp.2007.35.41.\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995, In AGARD, 390.\n\\bibitem[Nayfeh \\& Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H., \\& Balachandran, B.\\ 1995, Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995.\n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988, arXiv e-printshep-th/9108028.\n\\bibitem[Khatib, et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983, AIAA, Aerospace Sciences Meeting.\n\\bibitem[Thornton, et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219.\n"} +data_ASPC= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': "\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018, Weather, 73, 35. doi:10.1002/wea.3072.\n\\bibitem[Fal'ko \\& Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V., \\& Thomas, C.-W.\\ 2018, 2D Materials, 5, 010201. doi:10.1088/2053-1583/aa9403.\n\\bibitem[Parkin, et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018, Spin, 8, 1877001. doi:10.1142/S2010324718770015.\n\\bibitem[Dessauges-Zavadsky \\& Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M., \\& Pfenniger, D.\\ 2018, Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018, 38. doi:10.1007/978-3-662-57546-8.\n\\bibitem[Pustilnik, et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., et al.\\ 2018, \\prl, 120, 029901. doi:10.1103/PhysRevLett.120.029901.\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017, Ph.D. Thesis. doi:10.5281/zenodo.581221.\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017, AAS Nova Highlights, 2388.\n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017, Central Bureau Electronic Telegrams, 4403.\n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017, Astrophysics Source Code Library. ascl:1706.009.\n\\bibitem[Siltala, et al.(2017)]{2017yCat.113380453S} Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017, VizieR Online Data Catalog, J/AN/338/453.\n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017, AAVSO Special Notice \\#429, 429.\n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017, Spitzer Proposal, 13168.\n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017, Masters Thesis, 2.\n\\bibitem[Rotaru, et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016, http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian).\n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias.\n\\bibitem[Liu, et al.(2009)]{2009bcet.book...65L} Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009, Biophysics and the Challenges of Emerging Threats, 65. doi:10.1007/978-90-481-2368-1\\_5.\n\\bibitem[Mahabal, et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007, \\aas, 210, 21.04.\n\\bibitem[. \\& .(2007)]{2007RJPh....1...35.} ., S.~N.~A., \\& ., E.~C.~O.\\ 2007, Research Journal of Physics, 1, 35. doi:10.3923/rjp.2007.35.41.\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995, In AGARD, 390.\n\\bibitem[Nayfeh \\& Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H., \\& Balachandran, B.\\ 1995, Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995.\n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988, arXiv e-printshep-th/9108028.\n\\bibitem[Khatib, et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983, AIAA, Aerospace Sciences Meeting.\n\\bibitem[Thornton, et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219.\n\\bibitem[Dhaygude \\& Desai(2020)]{2020EPJC...80...96D} Dhaygude, A., \\& Desai, S.\\ 2020, European Physical Journal C. doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970.\n"} -data_APSJ= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': u"No author, {\\bf 73}, 35 (2018). doi:10.1002/wea.3072.\nV. Fal'ko and C.-W. Thomas, {\\bf 5}, 010201 (2018). doi:10.1088/2053-1583/aa9403.\nS. Parkin, R. Chantrell, and C.-R. Chang, {\\bf 8}, 1877001 (2018). doi:10.1142/S2010324718770015.\nM. Dessauges-Zavadsky and D. Pfenniger, {\\bf 38}, (2018). doi:10.1007/978-3-662-57546-8.\nM. Pustilnik, B. van Heck, R.~M. Lutchyn, and L.~I. Glazman, {\\bf 120}, 029901 (2018). doi:10.1103/PhysRevLett.120.029901.\nD. Carton, Resolving Gas-phase Metallicity in Galaxies, 2017. doi:10.5281/zenodo.581221.\nS. Kohler, 2388 (2017).\nD.~W.~E. Green, {\\bf 4403}, 2 (2017).\nA.~R. Casey, Astrophysics Source Code Library. ascl:1706.009.\nJ. Siltala, L. Jetsu, T. Hackman, G.~W. Henry, L. Immonen, P. Kajatkari, J. Lankinen, J. Lehtinen, S. Monira, S. Nikbakhsh, A. Viitanen, J. Viuho, and T. Willamo, J/AN/338/453 (2017).\nE.~O. Waagen, {\\bf 429}, 1 (2017).\nL. Yan, 13168 (2017).\nS. Azankpo, Surface Accuracy and Pointing Error Prediction of a 32 M Diameter Class Radio Astronomy Telescope, 2017.\nA. Rotaru, M. Pteancu, and C. Zaharia, (2016).\nS. Velasco, 872 (2016).\nC.~W. Liu, V.~Y. Alekseyev, J.~R. Allwardt, A.~J. Bankovich, B.~J. Cade-Menun, R.~W. Davis, L.-S. Du, K.~C. Garcia, D. Herschlag, C. Khosla, D.~A. Kraut, Q. Li, B. Null, J.~D. Puglisi, P.~A. Sigala, J.~F. Stebbins, and L. Varani, in 65. doi:10.1007/978-90-481-2368-1_5.\nA.~A. Mahabal, A.~J. Drake, S.~G. Djorgovski, C. Donalek, E. Glikman, M.~J. Graham, R. Williams, C. Baltay, D. Rabinowitz, PQ Team Caltech, Yale, NCSA, Indiana, and ., {\\bf 210}, 21.04 (2007).\nS.~N.~A. . and E.~C.~O. ., {\\bf 1}, 35 (2007). doi:10.3923/rjp.2007.35.41.\nJ.~L. Miller, in 390.\nA.~H. Nayfeh and B. Balachandran, {\\it Applied Nonlinear Dynamics: Analytical, Computational and Experimental Methods}.\nP. Ginsparg, hep-th/9108028 (1988).\nA.~R. Khatib, J. Ellis, J. French, G. Null, T. Yunck, and S. Wu, .\nP.~E. Thornton, M.~M. Thornton, B.~W. Mayer, N. Wilhelmi, Y. Wei, R. Devarakonda, and R. Cook, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219.\n"} +data_APSJ= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': u"No author, {\\bf 73}, 35 (2018). doi:10.1002/wea.3072.\nV. Fal'ko and C.-W. Thomas, {\\bf 5}, 010201 (2018). doi:10.1088/2053-1583/aa9403.\nS. Parkin, R. Chantrell, and C.-R. Chang, {\\bf 8}, 1877001 (2018). doi:10.1142/S2010324718770015.\nM. Dessauges-Zavadsky and D. Pfenniger, {\\bf 38}, (2018). doi:10.1007/978-3-662-57546-8.\nM. Pustilnik, B. van Heck, R.~M. Lutchyn, and L.~I. Glazman, {\\bf 120}, 029901 (2018). doi:10.1103/PhysRevLett.120.029901.\nD. Carton, Resolving Gas-phase Metallicity in Galaxies, 2017. doi:10.5281/zenodo.581221.\nS. Kohler, 2388 (2017).\nD.~W.~E. Green, {\\bf 4403}, 2 (2017).\nA.~R. Casey, Astrophysics Source Code Library. ascl:1706.009.\nJ. Siltala, L. Jetsu, T. Hackman, G.~W. Henry, L. Immonen, P. Kajatkari, J. Lankinen, J. Lehtinen, S. Monira, S. Nikbakhsh, A. Viitanen, J. Viuho, and T. Willamo, J/AN/338/453 (2017).\nE.~O. Waagen, {\\bf 429}, 1 (2017).\nL. Yan, 13168 (2017).\nS. Azankpo, Surface Accuracy and Pointing Error Prediction of a 32 M Diameter Class Radio Astronomy Telescope, 2017.\nA. Rotaru, M. Pteancu, and C. Zaharia, (2016).\nS. Velasco, 872 (2016).\nC.~W. Liu, V.~Y. Alekseyev, J.~R. Allwardt, A.~J. Bankovich, B.~J. Cade-Menun, R.~W. Davis, L.-S. Du, K.~C. Garcia, D. Herschlag, C. Khosla, D.~A. Kraut, Q. Li, B. Null, J.~D. Puglisi, P.~A. Sigala, J.~F. Stebbins, and L. Varani, in 65. doi:10.1007/978-90-481-2368-1_5.\nA.~A. Mahabal, A.~J. Drake, S.~G. Djorgovski, C. Donalek, E. Glikman, M.~J. Graham, R. Williams, C. Baltay, D. Rabinowitz, PQ Team Caltech, Yale, NCSA, Indiana, and ., {\\bf 210}, 21.04 (2007).\nS.~N.~A. . and E.~C.~O. ., {\\bf 1}, 35 (2007). doi:10.3923/rjp.2007.35.41.\nJ.~L. Miller, in 390.\nA.~H. Nayfeh and B. Balachandran, {\\it Applied Nonlinear Dynamics: Analytical, Computational and Experimental Methods}.\nP. Ginsparg, hep-th/9108028 (1988).\nA.~R. Khatib, J. Ellis, J. French, G. Null, T. Yunck, and S. Wu, .\nP.~E. Thornton, M.~M. Thornton, B.~W. Mayer, N. Wilhelmi, Y. Wei, R. Devarakonda, and R. Cook, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219.\nA. Dhaygude and S. Desai, (2020). doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970.\n"} -data_AASJ= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': u"\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018, Weather, 73, 35. doi:10.1002/wea.3072.\n\\bibitem[Fal'ko, \\& Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V., \\& Thomas, C.-W.\\ 2018, 2D Materials, 5, 010201. doi:10.1088/2053-1583/aa9403.\n\\bibitem[Parkin, et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018, Spin, 8, 1877001. doi:10.1142/S2010324718770015.\n\\bibitem[Dessauges-Zavadsky, \\& Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M., \\& Pfenniger, D.\\ 2018, Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018, 38. doi:10.1007/978-3-662-57546-8.\n\\bibitem[Pustilnik, et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., et al.\\ 2018, \\prl, 120, 029901. doi:10.1103/PhysRevLett.120.029901.\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017, Ph.D. Thesis. doi:10.5281/zenodo.581221.\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017, AAS Nova Highlights, 2388.\n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017, Central Bureau Electronic Telegrams, 4403.\n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017, Astrophysics Source Code Library. ascl:1706.009.\n\\bibitem[Siltala, et al.(2017)]{2017yCat.113380453S} Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017, VizieR Online Data Catalog, J/AN/338/453.\n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017, AAVSO Special Notice \\#429, 429.\n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017, Spitzer Proposal, 13168.\n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017, Masters Thesis, 2.\n\\bibitem[Rotaru, et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016, http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian).\n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias.\n\\bibitem[Liu, et al.(2009)]{2009bcet.book...65L} Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009, Biophysics and the Challenges of Emerging Threats, 65. doi:10.1007/978-90-481-2368-1\\_5.\n\\bibitem[Mahabal, et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007, \\aas.\n\\bibitem[., \\& .(2007)]{2007RJPh....1...35.} ., S.~N.~A., \\& ., E.~C.~O.\\ 2007, Research Journal of Physics, 1, 35. doi:10.3923/rjp.2007.35.41.\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995, In AGARD, 390.\n\\bibitem[Nayfeh, \\& Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H., \\& Balachandran, B.\\ 1995, Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995.\n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988, arXiv e-prints, hep-th/9108028.\n\\bibitem[Khatib, et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983, AIAA, Aerospace Sciences Meeting.\n\\bibitem[Thornton, et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219.\n"} +data_AASJ= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': u"\\bibitem[No author(2018)]{2018Wthr...73Q..35.} No author\\ 2018, Weather, 73, 35. doi:10.1002/wea.3072.\n\\bibitem[Fal'ko, \\& Thomas(2018)]{2018TDM.....5a0201F} Fal'ko, V., \\& Thomas, C.-W.\\ 2018, 2D Materials, 5, 010201. doi:10.1088/2053-1583/aa9403.\n\\bibitem[Parkin, et al.(2018)]{2018Spin....877001P} Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018, Spin, 8, 1877001. doi:10.1142/S2010324718770015.\n\\bibitem[Dessauges-Zavadsky, \\& Pfenniger(2018)]{2018SAAS...38.....D} Dessauges-Zavadsky, M., \\& Pfenniger, D.\\ 2018, Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018, 38. doi:10.1007/978-3-662-57546-8.\n\\bibitem[Pustilnik, et al.(2018)]{2018PhRvL.120b9901P} Pustilnik, M., van Heck, B., Lutchyn, R.~M., et al.\\ 2018, \\prl, 120, 029901. doi:10.1103/PhysRevLett.120.029901.\n\\bibitem[Carton(2017)]{2017PhDT........14C} Carton, D.\\ 2017, Ph.D. Thesis. doi:10.5281/zenodo.581221.\n\\bibitem[Kohler(2017)]{2017nova.pres.2388K} Kohler, S.\\ 2017, AAS Nova Highlights, 2388.\n\\bibitem[Green(2017)]{2017CBET.4403....2G} Green, D.~W.~E.\\ 2017, Central Bureau Electronic Telegrams, 4403.\n\\bibitem[Casey(2017)]{2017ascl.soft06009C} Casey, A.~R.\\ 2017, Astrophysics Source Code Library. ascl:1706.009.\n\\bibitem[Siltala, et al.(2017)]{2017yCat.113380453S} Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017, VizieR Online Data Catalog, J/AN/338/453.\n\\bibitem[Waagen(2017)]{2017AAVSN.429....1W} Waagen, E.~O.\\ 2017, AAVSO Special Notice \\#429, 429.\n\\bibitem[Yan(2017)]{2017sptz.prop13168Y} Yan, L.\\ 2017, Spitzer Proposal, 13168.\n\\bibitem[Azankpo(2017)]{2017MsT..........2A} Azankpo, S.\\ 2017, Masters Thesis, 2.\n\\bibitem[Rotaru, et al.(2016)]{2016emo6.rept.....R} Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016, http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian).\n\\bibitem[Velasco(2016)]{2016iac..talk..872V} Velasco, S.\\ 2016, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias.\n\\bibitem[Liu, et al.(2009)]{2009bcet.book...65L} Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009, Biophysics and the Challenges of Emerging Threats, 65. doi:10.1007/978-90-481-2368-1\\_5.\n\\bibitem[Mahabal, et al.(2007)]{2007AAS...210.2104M} Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007, \\aas.\n\\bibitem[., \\& .(2007)]{2007RJPh....1...35.} ., S.~N.~A., \\& ., E.~C.~O.\\ 2007, Research Journal of Physics, 1, 35. doi:10.3923/rjp.2007.35.41.\n\\bibitem[Miller(1995)]{1995ans..agar..390M} Miller, J.~L.\\ 1995, In AGARD, 390.\n\\bibitem[Nayfeh, \\& Balachandran(1995)]{1995anda.book.....N} Nayfeh, A.~H., \\& Balachandran, B.\\ 1995, Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995.\n\\bibitem[Ginsparg(1988)]{1991hep.th....8028G} Ginsparg, P.\\ 1988, arXiv e-prints, hep-th/9108028.\n\\bibitem[Khatib, et al.(1983)]{1983aiaa.meetY....K} Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983, AIAA, Aerospace Sciences Meeting.\n\\bibitem[Thornton, et al.(2012)]{2012ddsw.rept.....T} Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. doi:10.3334/ORNLDAAC/1219.\n\\bibitem[Dhaygude, \\& Desai(2020)]{2020EPJC...80...96D} Dhaygude, A., \\& Desai, S.\\ 2020, European Physical Journal C. doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970.\n"} -data_ieee= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': u"[1]No author, \u201cBook reviews\u201d, Weather, vol. 73, no. 1, pp. 35\u201335, 2018. doi:10.1002/wea.3072.\n[2]Fal'ko, V. and Thomas, C.-W., \u201c2D Materials: maintaining editorial quality\u201d, 2D Materials, vol. 5, no. 1, Art. no. 010201, 2018. doi:10.1088/2053-1583/aa9403.\n[3]Parkin, S., Chantrell, R., and Chang, C.-R., \u201cObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\u201d, Spin, vol. 8, no. 4, Art. no. 1877001, 2018. doi:10.1142/S2010324718770015.\n[4]Dessauges-Zavadsky, M. and Pfenniger, D., \u201cMillimeter Astronomy\u201d, SAAS...38, 2018. doi:10.1007/978-3-662-57546-8.\n[5]Pustilnik, M., van Heck, B., Lutchyn, R. M., and Glazman, L. I., \u201cErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\u201d, Physical Review Letters, vol. 120, no. 2, Art. no. 029901, 2018. doi:10.1103/PhysRevLett.120.029901.\n[6]Carton, D., \u201cResolving Gas-Phase Metallicity In Galaxies\u201d, PhDT, Leiden University, 2017. doi:10.5281/zenodo.581221.\n[7]Kohler, S., \u201cA 3D View of a Supernova Remnant\u201d, AAS Nova Highlights, Art. no. 2388, 2017.\n[8]Green, D. W. E., \u201cPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\u201d, CBET.4403, 2017.\n[9]Casey, A. R., \u201csick: Spectroscopic inference crank\u201d, Astrophysics Source Code Library, Art. no. ascl:1706.009, 2017. ascl:1706.009.\n[10]Siltala, J., \u201cVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\u201d, VizieR Online Data Catalog, Art. no. J/AN/338/453, 2017.\n[11]Waagen, E. O., \u201cV694 Mon (MWC 560) spectroscopy requested\u201d, AAVSN.429, 2017.\n[12]Yan, L., \u201cConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\u201d, Spitzer Proposal, p. 13168, 2017.\n[13]Azankpo, S., \u201cSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\u201d, MsT, University of Stellenbosch, 2017.\n[14]Rotaru, A., Pteancu, M., and Zaharia, C., \u201cThe penumbral Moon's eclipse form 16 september 2016\u201d, emo6.rept, 2016.\n[15]Velasco, S., \u201cLiving on the edge: Adaptive Optics+Lucky Imaging\u201d, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, p. 872, 2016.\n[16]Liu, C. W., \u201cThe Diversity of Nuclear Magnetic Resonance Spectroscopy\u201d, in Biophysics and the Challenges of Emerging Threats, J. D. Puglisi, Ed. 2009, p. 65. doi:10.1007/978-90-481-2368-1_5.\n[17]Mahabal, A. A., \u201cTime Domain Exploration with the Palomar-QUEST Sky Survey\u201d, vol. 210, Art. no. 21.04, 2007.\n[18]., S. N. A. and ., E. C. O., \u201cAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\u201d, Research Journal of Physics, vol. 1, no. 1, pp. 35\u201341, 2007. doi:10.3923/rjp.2007.35.41.\n[19]Miller, J. L., \u201cSpacecraft navigation requirements\u201d, in In AGARD, 1995, pp. 390\u2013405.\n[20]Nayfeh, A. H. and Balachandran, B., Applied nonlinear dynamics: analytical, computational and experimental methods. 1995.\n[21]Ginsparg, P., \u201cApplied Conformal Field Theory\u201d, arXiv e-prints, Art. no. hep-th/9108028, 1988.\n[22]Khatib, A. R., Ellis, J., French, J., Null, G., Yunck, T., and Wu, S., \u201cAutonomous navigation using lunar beacons\u201d, in AIAA, Aerospace Sciences Meeting, 1983.\n[23]Thornton, P. E., “Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008”, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC, 2012. doi:10.3334/ORNLDAAC/1219.\n"} +data_ieee= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': u"[1]No author, \u201cBook reviews\u201d, Weather, vol. 73, no. 1, pp. 35\u201335, 2018. doi:10.1002/wea.3072.\n[2]Fal'ko, V. and Thomas, C.-W., \u201c2D Materials: maintaining editorial quality\u201d, 2D Materials, vol. 5, no. 1, Art. no. 010201, 2018. doi:10.1088/2053-1583/aa9403.\n[3]Parkin, S., Chantrell, R., and Chang, C.-R., \u201cObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\u201d, Spin, vol. 8, no. 4, Art. no. 1877001, 2018. doi:10.1142/S2010324718770015.\n[4]Dessauges-Zavadsky, M. and Pfenniger, D., \u201cMillimeter Astronomy\u201d, SAAS...38, 2018. doi:10.1007/978-3-662-57546-8.\n[5]Pustilnik, M., van Heck, B., Lutchyn, R. M., and Glazman, L. I., \u201cErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\u201d, Physical Review Letters, vol. 120, no. 2, Art. no. 029901, 2018. doi:10.1103/PhysRevLett.120.029901.\n[6]Carton, D., \u201cResolving Gas-Phase Metallicity In Galaxies\u201d, PhDT, Leiden University, 2017. doi:10.5281/zenodo.581221.\n[7]Kohler, S., \u201cA 3D View of a Supernova Remnant\u201d, AAS Nova Highlights, Art. no. 2388, 2017.\n[8]Green, D. W. E., \u201cPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\u201d, CBET.4403, 2017.\n[9]Casey, A. R., \u201csick: Spectroscopic inference crank\u201d, Astrophysics Source Code Library, Art. no. ascl:1706.009, 2017. ascl:1706.009.\n[10]Siltala, J., \u201cVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\u201d, VizieR Online Data Catalog, Art. no. J/AN/338/453, 2017.\n[11]Waagen, E. O., \u201cV694 Mon (MWC 560) spectroscopy requested\u201d, AAVSN.429, 2017.\n[12]Yan, L., \u201cConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\u201d, Spitzer Proposal, p. 13168, 2017.\n[13]Azankpo, S., \u201cSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\u201d, MsT, University of Stellenbosch, 2017.\n[14]Rotaru, A., Pteancu, M., and Zaharia, C., \u201cThe penumbral Moon's eclipse form 16 september 2016\u201d, emo6.rept, 2016.\n[15]Velasco, S., \u201cLiving on the edge: Adaptive Optics+Lucky Imaging\u201d, IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, p. 872, 2016.\n[16]Liu, C. W., \u201cThe Diversity of Nuclear Magnetic Resonance Spectroscopy\u201d, in Biophysics and the Challenges of Emerging Threats, J. D. Puglisi, Ed. 2009, p. 65. doi:10.1007/978-90-481-2368-1_5.\n[17]Mahabal, A. A., \u201cTime Domain Exploration with the Palomar-QUEST Sky Survey\u201d, vol. 210, Art. no. 21.04, 2007.\n[18]., S. N. A. and ., E. C. O., \u201cAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\u201d, Research Journal of Physics, vol. 1, no. 1, pp. 35\u201341, 2007. doi:10.3923/rjp.2007.35.41.\n[19]Miller, J. L., \u201cSpacecraft navigation requirements\u201d, in In AGARD, 1995, pp. 390\u2013405.\n[20]Nayfeh, A. H. and Balachandran, B., Applied nonlinear dynamics: analytical, computational and experimental methods. 1995.\n[21]Ginsparg, P., \u201cApplied Conformal Field Theory\u201d, arXiv e-prints, Art. no. hep-th/9108028, 1988.\n[22]Khatib, A. R., Ellis, J., French, J., Null, G., Yunck, T., and Wu, S., \u201cAutonomous navigation using lunar beacons\u201d, in AIAA, Aerospace Sciences Meeting, 1983.\n[23]Thornton, P. E., “Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008”, Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC, 2012. doi:10.3334/ORNLDAAC/1219.\n[24]Dhaygude, A. and Desai, S., “Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL”, European Physical Journal C, 2020. doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970.\n"} -data_agu= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': "No author (2018) Book reviews Weather, 73(1), 35–35. https://doi.org/10.1002/wea.3072\nFal'ko, V., & Thomas, C.-W. (2018) 2D Materials: maintaining editorial quality 2D Materials, 5(1), 010201. https://doi.org/10.1088/2053-1583/aa9403\nParkin, S., Chantrell, R., & Chang, C.-R. (2018) Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor Spin, 8(4), 1877001. https://doi.org/10.1142/S2010324718770015\nDessauges-Zavadsky, M., & Pfenniger, D. (2018) Millimeter Astronomy (SAAS...38) Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018 (Vol. 38). https://doi.org/10.1007/978-3-662-57546-8\nPustilnik, M., van Heck, B., Lutchyn, R. M., & Glazman, L. I. (2018) Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)] Physical Review Letters, 120(2), 029901. https://doi.org/10.1103/PhysRevLett.120.029901\nCarton, D. (2017) Resolving Gas-Phase Metallicity In Galaxies (PhDT) Ph.D. Thesis, Leiden University. https://doi.org/10.5281/zenodo.581221\nKohler, S. (2017) A 3D View of a Supernova Remnant AAS Nova Highlights (2388).\nGreen, D. W. E. (2017) Potential New Meteor Shower from Comet C/2015 D4 (Borisov) (CBET.4403) Central Bureau Electronic Telegrams (Vol. 4403, p. 2).\nCasey, A. R. (2017) sick: Spectroscopic inference crank Astrophysics Source Code Library. ascl:1706.009\nSiltala, J., Jetsu, L., Hackman, T., Henry, G. W., Immonen, L., Kajatkari, P., et al. (2017) VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017) VizieR Online Data Catalog (J/AN/338/453).\nWaagen, E. O. (2017) V694 Mon (MWC 560) spectroscopy requested (AAVSN.429) AAVSO Special Notice #429 (Vol. 429, p. 1).\nYan, L. (2017) Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves Spitzer Proposal, 13168.\nAzankpo, S. (2017) Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope (MsT) Masters Thesis, University of Stellenbosch.\nRotaru, A., Pteancu, M., & Zaharia, C. (2016) The penumbral Moon's eclipse form 16 september 2016 (emo6.rept) http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian).\nVelasco, S. (2016) Living on the edge: Adaptive Optics+Lucky Imaging IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, p. 872.\nLiu, C. W., Alekseyev, V. Y., Allwardt, J. R., Bankovich, A. J., Cade-Menun, B. J., Davis, R. W., et al. (2009) The Diversity of Nuclear Magnetic Resonance Spectroscopy In J. D. Puglisi (Ed.), Biophysics and the Challenges of Emerging Threats (p. 65). https://doi.org/10.1007/978-90-481-2368-1_5\nMahabal, A. A., Drake, A. J., Djorgovski, S. G., Donalek, C., Glikman, E., Graham, M. J., et al. (2007) Time Domain Exploration with the Palomar-QUEST Sky Survey American Astronomical Society Meeting Abstracts #210, 210, 21.04.\n., S. N. A., & ., E. C. O. (2007) Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater Research Journal of Physics, 1(1), 35–41. https://doi.org/10.3923/rjp.2007.35.41\nMiller, J. L. (1995) Spacecraft navigation requirements In In AGARD (pp. 390–405).\nNayfeh, A. H., & Balachandran, B. (1995) Applied nonlinear dynamics: analytical, computational and experimental methods Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995.\nGinsparg, P. (1988) Applied Conformal Field Theory arXiv e-prints (hep-th/9108028).\nKhatib, A. R., Ellis, J., French, J., Null, G., Yunck, T., & Wu, S. (1983) Autonomous navigation using lunar beacons In AIAA, Aerospace Sciences Meeting.\nThornton, P. E., Thornton, M. M., Mayer, B. W., Wilhelmi, N., Wei, Y., Devarakonda, R., & Cook, R. (2012) Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008 Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. 10.3334/ORNLDAAC/1219\n"} +data_agu= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': "No author (2018) Book reviews Weather, 73(1), 35–35. https://doi.org/10.1002/wea.3072\nFal'ko, V., & Thomas, C.-W. (2018) 2D Materials: maintaining editorial quality 2D Materials, 5(1), 010201. https://doi.org/10.1088/2053-1583/aa9403\nParkin, S., Chantrell, R., & Chang, C.-R. (2018) Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor Spin, 8(4), 1877001. https://doi.org/10.1142/S2010324718770015\nDessauges-Zavadsky, M., & Pfenniger, D. (2018) Millimeter Astronomy (SAAS...38) Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018 (Vol. 38). https://doi.org/10.1007/978-3-662-57546-8\nPustilnik, M., van Heck, B., Lutchyn, R. M., & Glazman, L. I. (2018) Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)] Physical Review Letters, 120(2), 029901. https://doi.org/10.1103/PhysRevLett.120.029901\nCarton, D. (2017) Resolving Gas-Phase Metallicity In Galaxies (PhDT) Ph.D. Thesis, Leiden University. https://doi.org/10.5281/zenodo.581221\nKohler, S. (2017) A 3D View of a Supernova Remnant AAS Nova Highlights (2388).\nGreen, D. W. E. (2017) Potential New Meteor Shower from Comet C/2015 D4 (Borisov) (CBET.4403) Central Bureau Electronic Telegrams (Vol. 4403, p. 2).\nCasey, A. R. (2017) sick: Spectroscopic inference crank Astrophysics Source Code Library. ascl:1706.009\nSiltala, J., Jetsu, L., Hackman, T., Henry, G. W., Immonen, L., Kajatkari, P., et al. (2017) VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017) VizieR Online Data Catalog (J/AN/338/453).\nWaagen, E. O. (2017) V694 Mon (MWC 560) spectroscopy requested (AAVSN.429) AAVSO Special Notice #429 (Vol. 429, p. 1).\nYan, L. (2017) Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves Spitzer Proposal, 13168.\nAzankpo, S. (2017) Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope (MsT) Masters Thesis, University of Stellenbosch.\nRotaru, A., Pteancu, M., & Zaharia, C. (2016) The penumbral Moon's eclipse form 16 september 2016 (emo6.rept) http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian).\nVelasco, S. (2016) Living on the edge: Adaptive Optics+Lucky Imaging IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, p. 872.\nLiu, C. W., Alekseyev, V. Y., Allwardt, J. R., Bankovich, A. J., Cade-Menun, B. J., Davis, R. W., et al. (2009) The Diversity of Nuclear Magnetic Resonance Spectroscopy In J. D. Puglisi (Ed.), Biophysics and the Challenges of Emerging Threats (p. 65). https://doi.org/10.1007/978-90-481-2368-1_5\nMahabal, A. A., Drake, A. J., Djorgovski, S. G., Donalek, C., Glikman, E., Graham, M. J., et al. (2007) Time Domain Exploration with the Palomar-QUEST Sky Survey American Astronomical Society Meeting Abstracts #210, 210, 21.04.\n., S. N. A., & ., E. C. O. (2007) Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater Research Journal of Physics, 1(1), 35–41. https://doi.org/10.3923/rjp.2007.35.41\nMiller, J. L. (1995) Spacecraft navigation requirements In In AGARD (pp. 390–405).\nNayfeh, A. H., & Balachandran, B. (1995) Applied nonlinear dynamics: analytical, computational and experimental methods Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995.\nGinsparg, P. (1988) Applied Conformal Field Theory arXiv e-prints (hep-th/9108028).\nKhatib, A. R., Ellis, J., French, J., Null, G., Yunck, T., & Wu, S. (1983) Autonomous navigation using lunar beacons In AIAA, Aerospace Sciences Meeting.\nThornton, P. E., Thornton, M. M., Mayer, B. W., Wilhelmi, N., Wei, Y., Devarakonda, R., & Cook, R. (2012) Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008 Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC. 10.3334/ORNLDAAC/1219\nDhaygude, A., & Desai, S. (2020) Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL European Physical Journal C. https://doi.org/10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\n"} -data_gsa= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': "No author, 2018, Book reviews: Weather, v. 73, p. 35–35, doi:10.1002/wea.3072.\nFal'ko, V., and Thomas, C.-W., 2018, 2D Materials: maintaining editorial quality: 2D Materials, v. 5, 010201, doi:10.1088/2053-1583/aa9403.\nParkin, S., Chantrell, R., and Chang, C.-R., 2018, Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor: Spin, v. 8, 1877001, doi:10.1142/S2010324718770015.\nDessauges-Zavadsky, M., and Pfenniger, D., 2018, Millimeter Astronomy: SAAS...38, doi:10.1007/978-3-662-57546-8.\nPustilnik, M., van Heck, B., Lutchyn, R.M., and Glazman, L.I., 2018, Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]: Physical Review Letters, v. 120, 029901, doi:10.1103/PhysRevLett.120.029901.\nCarton, D., 2017, Resolving Gas-Phase Metallicity In Galaxies [PhDT], doi:10.5281/zenodo.581221.\nKohler, S., 2017, A 3D View of a Supernova Remnant: AAS Nova Highlights, 2388.\nGreen, D.W.E., 2017, Potential New Meteor Shower from Comet C/2015 D4 (Borisov): CBET.4403, 2 p.\nCasey, A.R., 2017, sick: Spectroscopic inference crank: Astrophysics Source Code Library, ascl:1706.009, ascl:1706.009.\nSiltala, J. et al., 2017, VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017): VizieR Online Data Catalog, J/AN/338/453.\nWaagen, E.O., 2017, V694 Mon (MWC 560) spectroscopy requested: AAVSN.429, 1 p.\nYan, L., 2017, Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves: Spitzer Proposal, p. 13168.\nAzankpo, S., 2017, Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope [MsT].\nRotaru, A., Pteancu, M., and Zaharia, C., 2016, The penumbral Moon's eclipse form 16 september 2016: emo6.rept.\nVelasco, S., 2016, Living on the edge: Adaptive Optics+Lucky Imaging: IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, p. 872.\nLiu, C.W. et al., 2009, The Diversity of Nuclear Magnetic Resonance Spectroscopy, in Puglisi, J.D. ed., Biophysics and the Challenges of Emerging Threats, doi:10.1007/978-90-481-2368-1_5.\nMahabal, A.A. et al., 2007, Time Domain Exploration with the Palomar-QUEST Sky Survey: American Astronomical Society Meeting Abstracts #210, v. 210, 21.04.\n., S.N.A., and ., E.C.O., 2007, Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater: Research Journal of Physics, v. 1, p. 35–41, doi:10.3923/rjp.2007.35.41.\nMiller, J.L., 1995, Spacecraft navigation requirements, in In AGARD.\nNayfeh, A.H., and Balachandran, B., 1995, Applied nonlinear dynamics: analytical, computational and experimental methods.\nGinsparg, P., 1988, Applied Conformal Field Theory: arXiv e-prints, hep-th/9108028.\nKhatib, A.R., Ellis, J., French, J., Null, G., Yunck, T., and Wu, S., 1983, Autonomous navigation using lunar beacons, in AIAA, Aerospace Sciences Meeting.\nThornton, P.E., Thornton, M.M., Mayer, B.W., Wilhelmi, N., Wei, Y., Devarakonda, R., and Cook, R., 2012, Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008: Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC,, 10.3334/ORNLDAAC/1219.\n"} +data_gsa= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': "No author, 2018, Book reviews: Weather, v. 73, p. 35–35, doi:10.1002/wea.3072.\nFal'ko, V., and Thomas, C.-W., 2018, 2D Materials: maintaining editorial quality: 2D Materials, v. 5, 010201, doi:10.1088/2053-1583/aa9403.\nParkin, S., Chantrell, R., and Chang, C.-R., 2018, Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor: Spin, v. 8, 1877001, doi:10.1142/S2010324718770015.\nDessauges-Zavadsky, M., and Pfenniger, D., 2018, Millimeter Astronomy: SAAS...38, doi:10.1007/978-3-662-57546-8.\nPustilnik, M., van Heck, B., Lutchyn, R.M., and Glazman, L.I., 2018, Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]: Physical Review Letters, v. 120, 029901, doi:10.1103/PhysRevLett.120.029901.\nCarton, D., 2017, Resolving Gas-Phase Metallicity In Galaxies [PhDT], doi:10.5281/zenodo.581221.\nKohler, S., 2017, A 3D View of a Supernova Remnant: AAS Nova Highlights, 2388.\nGreen, D.W.E., 2017, Potential New Meteor Shower from Comet C/2015 D4 (Borisov): CBET.4403, 2 p.\nCasey, A.R., 2017, sick: Spectroscopic inference crank: Astrophysics Source Code Library, ascl:1706.009, ascl:1706.009.\nSiltala, J. et al., 2017, VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017): VizieR Online Data Catalog, J/AN/338/453.\nWaagen, E.O., 2017, V694 Mon (MWC 560) spectroscopy requested: AAVSN.429, 1 p.\nYan, L., 2017, Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves: Spitzer Proposal, p. 13168.\nAzankpo, S., 2017, Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope [MsT].\nRotaru, A., Pteancu, M., and Zaharia, C., 2016, The penumbral Moon's eclipse form 16 september 2016: emo6.rept.\nVelasco, S., 2016, Living on the edge: Adaptive Optics+Lucky Imaging: IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, p. 872.\nLiu, C.W. et al., 2009, The Diversity of Nuclear Magnetic Resonance Spectroscopy, in Puglisi, J.D. ed., Biophysics and the Challenges of Emerging Threats, doi:10.1007/978-90-481-2368-1_5.\nMahabal, A.A. et al., 2007, Time Domain Exploration with the Palomar-QUEST Sky Survey: American Astronomical Society Meeting Abstracts #210, v. 210, 21.04.\n., S.N.A., and ., E.C.O., 2007, Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater: Research Journal of Physics, v. 1, p. 35–41, doi:10.3923/rjp.2007.35.41.\nMiller, J.L., 1995, Spacecraft navigation requirements, in In AGARD.\nNayfeh, A.H., and Balachandran, B., 1995, Applied nonlinear dynamics: analytical, computational and experimental methods.\nGinsparg, P., 1988, Applied Conformal Field Theory: arXiv e-prints, hep-th/9108028.\nKhatib, A.R., Ellis, J., French, J., Null, G., Yunck, T., and Wu, S., 1983, Autonomous navigation using lunar beacons, in AIAA, Aerospace Sciences Meeting.\nThornton, P.E., Thornton, M.M., Mayer, B.W., Wilhelmi, N., Wei, Y., Devarakonda, R., and Cook, R., 2012, Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008: Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC,, 10.3334/ORNLDAAC/1219.\nDhaygude, A., and Desai, S., 2020, Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL: European Physical Journal C,, doi:10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970.\n"} -data_ams= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': "No author, 2018: Book reviews 73, 35–35, https://doi.org/10.1002/wea.3072.\nFal'ko, V., and C.-W. Thomas, 2018: 2D Materials: maintaining editorial quality 5, 010201, https://doi.org/10.1088/2053-1583/aa9403.\nParkin, S., R. Chantrell, and C.-R. Chang, 2018: Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor 8, 1877001, https://doi.org/10.1142/S2010324718770015.\nDessauges-Zavadsky, M., and D. Pfenniger, 2018: Millimeter Astronomy 38, https://doi.org/10.1007/978-3-662-57546-8.\nPustilnik, M., B. van Heck, R. M. Lutchyn, and L. I. Glazman, 2018: Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)] 120, 029901, https://doi.org/10.1103/PhysRevLett.120.029901.\nCarton, D., 2017: Resolving Gas-Phase Metallicity In Galaxies https://doi.org/10.5281/zenodo.581221.\nKohler, S., 2017: A 3D View of a Supernova Remnant 2388.\nGreen, D. W. E., 2017: Potential New Meteor Shower from Comet C/2015 D4 (Borisov) 4403, 2.\nCasey, A. R., 2017: sick: Spectroscopic inference crank ascl:1706.009, ascl:1706.009.\nSiltala, J., 2017: VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017) J/AN/338/453.\nWaagen, E. O., 2017: V694 Mon (MWC 560) spectroscopy requested 429, 1.\nYan, L., 2017: Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves 13168.\nAzankpo, S., 2017: Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope 2.\nRotaru, A., M. Pteancu, and C. Zaharia, 2016: The penumbral Moon's eclipse form 16 september 2016.\nVelasco, S., 2016: Living on the edge: Adaptive Optics+Lucky Imaging 872.\nLiu, C. W., 2009: The Diversity of Nuclear Magnetic Resonance Spectroscopy. Biophysics and the Challenges of Emerging Threats, J.D. Puglisi, Ed., p. 65, https://doi.org/10.1007/978-90-481-2368-1_5.\nMahabal, A. A., 2007: Time Domain Exploration with the Palomar-QUEST Sky Survey 210, 21.04.\n., S. N. A., and E. C. O. ., 2007: Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater 1, 35–41, https://doi.org/10.3923/rjp.2007.35.41.\nMiller, J. L., 1995: Spacecraft navigation requirements. In AGARD, 390–405.\nNayfeh, A. H., and B. Balachandran, 1995: Applied nonlinear dynamics: analytical, computational and experimental methods.\nGinsparg, P., 1988: Applied Conformal Field Theory hep-th/9108028.\nKhatib, A. R., J. Ellis, J. French, G. Null, T. Yunck, and S. Wu, 1983: Autonomous navigation using lunar beacons. AIAA, Aerospace Sciences Meeting.\nThornton, P. E., M. M. Thornton, B. W. Mayer, N. Wilhelmi, Y. Wei, R. Devarakonda, and R. Cook, 2012: Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008, 10.3334/ORNLDAAC/1219.\n"} +data_ams= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': "No author, 2018: Book reviews 73, 35–35, https://doi.org/10.1002/wea.3072.\nFal'ko, V., and C.-W. Thomas, 2018: 2D Materials: maintaining editorial quality 5, 010201, https://doi.org/10.1088/2053-1583/aa9403.\nParkin, S., R. Chantrell, and C.-R. Chang, 2018: Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor 8, 1877001, https://doi.org/10.1142/S2010324718770015.\nDessauges-Zavadsky, M., and D. Pfenniger, 2018: Millimeter Astronomy 38, https://doi.org/10.1007/978-3-662-57546-8.\nPustilnik, M., B. van Heck, R. M. Lutchyn, and L. I. Glazman, 2018: Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)] 120, 029901, https://doi.org/10.1103/PhysRevLett.120.029901.\nCarton, D., 2017: Resolving Gas-Phase Metallicity In Galaxies https://doi.org/10.5281/zenodo.581221.\nKohler, S., 2017: A 3D View of a Supernova Remnant 2388.\nGreen, D. W. E., 2017: Potential New Meteor Shower from Comet C/2015 D4 (Borisov) 4403, 2.\nCasey, A. R., 2017: sick: Spectroscopic inference crank ascl:1706.009, ascl:1706.009.\nSiltala, J., 2017: VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017) J/AN/338/453.\nWaagen, E. O., 2017: V694 Mon (MWC 560) spectroscopy requested 429, 1.\nYan, L., 2017: Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves 13168.\nAzankpo, S., 2017: Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope 2.\nRotaru, A., M. Pteancu, and C. Zaharia, 2016: The penumbral Moon's eclipse form 16 september 2016.\nVelasco, S., 2016: Living on the edge: Adaptive Optics+Lucky Imaging 872.\nLiu, C. W., 2009: The Diversity of Nuclear Magnetic Resonance Spectroscopy. Biophysics and the Challenges of Emerging Threats, J.D. Puglisi, Ed., p. 65, https://doi.org/10.1007/978-90-481-2368-1_5.\nMahabal, A. A., 2007: Time Domain Exploration with the Palomar-QUEST Sky Survey 210, 21.04.\n., S. N. A., and E. C. O. ., 2007: Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater 1, 35–41, https://doi.org/10.3923/rjp.2007.35.41.\nMiller, J. L., 1995: Spacecraft navigation requirements. In AGARD, 390–405.\nNayfeh, A. H., and B. Balachandran, 1995: Applied nonlinear dynamics: analytical, computational and experimental methods.\nGinsparg, P., 1988: Applied Conformal Field Theory hep-th/9108028.\nKhatib, A. R., J. Ellis, J. French, G. Null, T. Yunck, and S. Wu, 1983: Autonomous navigation using lunar beacons. AIAA, Aerospace Sciences Meeting.\nThornton, P. E., M. M. Thornton, B. W. Mayer, N. Wilhelmi, Y. Wei, R. Devarakonda, and R. Cook, 2012: Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008, 10.3334/ORNLDAAC/1219.\nDhaygude, A., and S. Desai, 2020: Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL https://doi.org/10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970.\n"} diff --git a/exportsrv/tests/unittests/stubdata/customTest.py b/exportsrv/tests/unittests/stubdata/customTest.py index 54661e6..6f9854c 100644 --- a/exportsrv/tests/unittests/stubdata/customTest.py +++ b/exportsrv/tests/unittests/stubdata/customTest.py @@ -1,5 +1,5 @@ # -*- coding: utf-8 -*- -data= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': u"\\bibitem[No author\\(2018)]{No author2018}\\ No author\\ 2018\\,Weather\\,73\\,35 \n\\bibitem[Fal'ko \\& Thomas\\(2018)]{Fal'ko and Thomas2018}\\ Fal'ko, V., \\& Thomas, C.-W.\\ 2018\\,2D Materials\\,5\\,010201 \n\\bibitem[Parkin et al.\\(2018)]{Parkin2018}\\ Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018\\,Spin\\,8\\,1877001 \n\\bibitem[Dessauges-Zavadsky \\& Pfenniger\\(2018)]{Dessauges-Zavadsky and Pfenniger2018}\\ Dessauges-Zavadsky, M., \\& Pfenniger, D.\\ 2018\\,Saas-Fee Advanced Course\\,38 \n\\bibitem[Pustilnik et al.\\(2018)]{Pustilnik2018}\\ Pustilnik, M., van Heck, B., Lutchyn, R.~M., \\& Glazman, L.~I.\\ 2018\\,\\prl\\,120\\,029901 \n\\bibitem[Carton\\(2017)]{Carton2017}\\ Carton, D.\\ 2017\\,Ph.D. Thesis \n\\bibitem[Kohler\\(2017)]{Kohler2017}\\ Kohler, S.\\ 2017\\,AAS Nova Highlights\\,2388 \n\\bibitem[Green\\(2017)]{Green2017}\\ Green, D.~W.~E.\\ 2017\\,Central Bureau Electronic Telegrams\\,4403\\,2 \n\\bibitem[Casey\\(2017)]{Casey2017}\\ Casey, A.~R.\\ 2017\\,Astrophysics Source Code Library\\,ascl:1706.009 \n\\bibitem[Siltala et al.\\(2017)]{Siltala2017}\\ Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017\\,VizieR Online Data Catalog\\,J/AN/338/453 \n\\bibitem[Waagen\\(2017)]{Waagen2017}\\ Waagen, E.~O.\\ 2017\\,AAVSO Special Notice\\,429\\,1 \n\\bibitem[Yan\\(2017)]{Yan2017}\\ Yan, L.\\ 2017\\,Spitzer Proposal\\,13168 \n\\bibitem[Azankpo\\(2017)]{Azankpo2017}\\ Azankpo, S.\\ 2017\\,Masters Thesis\\,2 \n\\bibitem[Rotaru et al.\\(2016)]{Rotaru2016}\\ Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016\\,http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian \n\\bibitem[Velasco\\(2016)]{Velasco2016}\\ Velasco, S.\\ 2016\\,IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias\\,872 \n\\bibitem[Liu et al.\\(2009)]{Liu2009}\\ Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009\\,Biophysics and the Challenges of Emerging Threats\\,65 \n\\bibitem[Mahabal et al.\\(2007)]{Mahabal2007}\\ Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007\\,\\aas\\,210\\,21.04 \n\\bibitem[. \\& .\\(2007)]{. and .2007}\\ ., S.~N.~A., \\& ., E.~C.~O.\\ 2007\\,Research Journal of Physics\\,1\\,35 \n\\bibitem[Miller\\(1995)]{Miller1995}\\ Miller, J.~L.\\ 1995\\,In AGARD\\,390 \n\\bibitem[Nayfeh \\& Balachandran\\(1995)]{Nayfeh and Balachandran1995}\\ Nayfeh, A.~H., \\& Balachandran, B.\\ 1995\\,Wiley series in nonlinear science \n\\bibitem[Ginsparg\\(1988)]{Ginsparg1988}\\ Ginsparg, P.\\ 1988\\,arXiv e-prints\\,hep-th/9108028 \n\\bibitem[Khatib et al.\\(1983)]{Khatib1983}\\ Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983\\,AIAA, Aerospace Sciences Meeting \n\\bibitem[Thornton et al.\\(2012)]{Thornton2012}\\ Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012\\,Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC \n"} +data= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': u"\\bibitem[No author\\(2018)]{No author2018}\\ No author\\ 2018\\,Weather\\,73\\,35 \n\\bibitem[Fal'ko \\& Thomas\\(2018)]{Fal'ko and Thomas2018}\\ Fal'ko, V., \\& Thomas, C.-W.\\ 2018\\,2D Materials\\,5\\,010201 \n\\bibitem[Parkin et al.\\(2018)]{Parkin2018}\\ Parkin, S., Chantrell, R., \\& Chang, C.-R.\\ 2018\\,Spin\\,8\\,1877001 \n\\bibitem[Dessauges-Zavadsky \\& Pfenniger\\(2018)]{Dessauges-Zavadsky and Pfenniger2018}\\ Dessauges-Zavadsky, M., \\& Pfenniger, D.\\ 2018\\,Saas-Fee Advanced Course\\,38 \n\\bibitem[Pustilnik et al.\\(2018)]{Pustilnik2018}\\ Pustilnik, M., van Heck, B., Lutchyn, R.~M., \\& Glazman, L.~I.\\ 2018\\,\\prl\\,120\\,029901 \n\\bibitem[Carton\\(2017)]{Carton2017}\\ Carton, D.\\ 2017\\,Ph.D. Thesis \n\\bibitem[Kohler\\(2017)]{Kohler2017}\\ Kohler, S.\\ 2017\\,AAS Nova Highlights\\,2388 \n\\bibitem[Green\\(2017)]{Green2017}\\ Green, D.~W.~E.\\ 2017\\,Central Bureau Electronic Telegrams\\,4403\\,2 \n\\bibitem[Casey\\(2017)]{Casey2017}\\ Casey, A.~R.\\ 2017\\,Astrophysics Source Code Library\\,ascl:1706.009 \n\\bibitem[Siltala et al.\\(2017)]{Siltala2017}\\ Siltala, J., Jetsu, L., Hackman, T., et al.\\ 2017\\,VizieR Online Data Catalog\\,J/AN/338/453 \n\\bibitem[Waagen\\(2017)]{Waagen2017}\\ Waagen, E.~O.\\ 2017\\,AAVSO Special Notice\\,429\\,1 \n\\bibitem[Yan\\(2017)]{Yan2017}\\ Yan, L.\\ 2017\\,Spitzer Proposal\\,13168 \n\\bibitem[Azankpo\\(2017)]{Azankpo2017}\\ Azankpo, S.\\ 2017\\,Masters Thesis\\,2 \n\\bibitem[Rotaru et al.\\(2016)]{Rotaru2016}\\ Rotaru, A., Pteancu, M., \\& Zaharia, C.\\ 2016\\,http://www.astronomy.ro/forum/viewtopic.php?p=159287\\#159287 (Comments in Romanian \n\\bibitem[Velasco\\(2016)]{Velasco2016}\\ Velasco, S.\\ 2016\\,IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof\\ísica de Canarias\\,872 \n\\bibitem[Liu et al.\\(2009)]{Liu2009}\\ Liu, C.~W., Alekseyev, V.~Y., Allwardt, J.~R., et al.\\ 2009\\,Biophysics and the Challenges of Emerging Threats\\,65 \n\\bibitem[Mahabal et al.\\(2007)]{Mahabal2007}\\ Mahabal, A.~A., Drake, A.~J., Djorgovski, S.~G., et al.\\ 2007\\,\\aas\\,210\\,21.04 \n\\bibitem[. \\& .\\(2007)]{. and .2007}\\ ., S.~N.~A., \\& ., E.~C.~O.\\ 2007\\,Research Journal of Physics\\,1\\,35 \n\\bibitem[Miller\\(1995)]{Miller1995}\\ Miller, J.~L.\\ 1995\\,In AGARD\\,390 \n\\bibitem[Nayfeh \\& Balachandran\\(1995)]{Nayfeh and Balachandran1995}\\ Nayfeh, A.~H., \\& Balachandran, B.\\ 1995\\,Wiley series in nonlinear science \n\\bibitem[Ginsparg\\(1988)]{Ginsparg1988}\\ Ginsparg, P.\\ 1988\\,arXiv e-prints\\,hep-th/9108028 \n\\bibitem[Khatib et al.\\(1983)]{Khatib1983}\\ Khatib, A.~R., Ellis, J., French, J., et al.\\ 1983\\,AIAA, Aerospace Sciences Meeting \n\\bibitem[Thornton et al.\\(2012)]{Thornton2012}\\ Thornton, P.~E., Thornton, M.~M., Mayer, B.~W., et al.\\ 2012\\,Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC \n\\bibitem[Dhaygude \\& Desai\\(2020)]{Dhaygude and Desai2020}\\ Dhaygude, A., \\& Desai, S.\\ 2020\\,European Physical Journal C \n"} data_publisher= {'msg': 'Retrieved 5 abstracts, starting with number 1.', 'export': '\\bibitem[Schade\\(2024)]{Schade2024}\\ Schade, R.\\ 2024\\,Zenodo\\,Publisher:Zenodo \n\\bibitem[Vidmachenko\\(2024)]{Vidmachenko2024}\\ Vidmachenko, A.\\ 2024\\,Proceedings of the VIII International Scientific and Practical Conference. World science priorities (February 08 {\\textendash} 09\\,20\\,Publisher:World of Conferences \n\\bibitem[Vidmachenko\\(2024)]{Vidmachenko2024}\\ Vidmachenko, A.\\ 2024\\,In book: Astronomical almanac\\,204\\,Publisher:Kyiv \n\\bibitem[Kent\\(2018)]{Kent2018}\\ Kent, B.~R.\\ 2018\\,Science and Computing with Raspberry Pi\\,Publisher:Morgan \\& Claypool \n\\bibitem[Renwick\\(2023)]{Renwick2023}\\ Renwick, J.~A.\\ 2023\\,Under the weather: a future forecast for New Zealand\\,Publisher:HarperCollins \n'} \ No newline at end of file diff --git a/exportsrv/tests/unittests/stubdata/fieldedTest.py b/exportsrv/tests/unittests/stubdata/fieldedTest.py index d9a11d8..481e956 100755 --- a/exportsrv/tests/unittests/stubdata/fieldedTest.py +++ b/exportsrv/tests/unittests/stubdata/fieldedTest.py @@ -1,16 +1,16 @@ # -*- coding: utf-8 -*- -data_ads = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '%R 2018Wthr...73Q..35.\n%T Book reviews\n%J Weather\n%V 73\n%D 01/2018\n%P 35\n%L 35\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\n%B Not Available

\n%Y DOI: 10.1002/wea.3072\n\n\n%R 2018TDM.....5a0201F\n%T 2D Materials: maintaining editorial quality\n%A Fal\'ko, Vladimir; Thomas, Ceri-Wyn\n%F AA(Editor in Chief, National Graphene Institute, University of\nManchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol,\nUnited Kingdom)\n%J 2D Materials\n%V 5\n%D 01/2018\n%P 010201\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\n%B Not Available

\n%Y DOI: 10.1088/2053-1583/aa9403\n\n\n%R 2018Spin....877001P\n%T Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\n%A Parkin, Stuart; Chantrell, Roy; Chang, Ching-Ray\n%J Spin\n%V 8\n%D 01/2018\n%P 1877001\n%C (c) 2018: World Scientific Publishing Company\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%I PUB_PDF: Publisher PDF;\n%U https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\n%B Not Available

\n%Y DOI: 10.1142/S2010324718770015\n\n\n%R 2018SAAS...38.....D\n%T Millimeter Astronomy\n%A Dessauges-Zavadsky, Miroslava; Pfenniger, Daniel\n%J Saas-Fee Advanced Course\n%V 38\n%D 01/2018\n%K Physics\n%C (c) 2018: Springer-Verlag GmbH Germany, part of Springer Nature\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%I TOC: Table of Contents;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\n%B Not Available

\n%Y DOI: 10.1007/978-3-662-57546-8\n\n\n%R 2018PhRvL.120b9901P\n%T Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\n%A Pustilnik, M.; van Heck, B.; Lutchyn, R. M.; Glazman, L. I.\n%J Physical Review Letters\n%V 120\n%D 01/2018\n%P 029901\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\n%B Not Available

\n%Y DOI: 10.1103/PhysRevLett.120.029901\n\n\n%R 2017PhDT........14C\n%T Resolving Gas-Phase Metallicity In Galaxies\n%A Carton, David\n%F AA(Leiden University)\n%J Ph.D. Thesis\n%D 06/2017\n%K galaxies: evolution, galaxies: abundances, galaxies: ISM\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\n%B Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\n%Y DOI: 10.5281/zenodo.581221\n\n\n%R 2017nova.pres.2388K\n%T A 3D View of a Supernova Remnant\n%A Kohler, Susanna\n%J AAS Nova Highlights\n%D 06/2017\n%P 2388\n%K Features, Highlights, interstellar medium, stellar evolution,\nsupernova remnant, supernovae, white dwarfs\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\n%B The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\n\n\n%R 2017CBET.4403....2G\n%T Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\n%A Green, D. W. E.\n%J Central Bureau Electronic Telegrams\n%V 4403\n%D 06/2017\n%P 2\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\n%B A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\n\n\n%R 2017ascl.soft06009C\n%T sick: Spectroscopic inference crank\n%A Casey, Andrew R.\n%J Astrophysics Source Code Library\n%D 06/2017\n%P ascl:1706.009\n%K Software\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\n%B sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\n%Y eprintid: ascl:1706.009\n\n\n%R 2017yCat.113380453S\n%T VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\n%A Siltala, J.; Jetsu, L.; Hackman, T.; Henry, G. W.; Immonen, L.;\nKajatkari, P.; Lankinen, J.; Lehtinen, J.; Monira, S.; Nikbakhsh, S.;\nViitanen, A.; Viuho, J.; Willamo, T.\n%J VizieR Online Data Catalog\n%D 05/2017\n%P J/AN/338/453\n%K Stars: variable\n%I ABSTRACT: Abstract;\n%I Vizier: VizieR Catalog Service;\n%U https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\n%X phot.dat 2930x19 Differential photometry of BM CVn; phot_mlc.dat 2930x19\nDifferential photometry of BM CVn with MLC removed; res.dat 1319x185\n*Numerical results of the CPS analysis; res_mlc.dat 1319x185 *Results of\nthe CPS analysis with MLC removed\n%B The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\n\n\n%R 2017AAVSN.429....1W\n%T V694 Mon (MWC 560) spectroscopy requested\n%A Waagen, Elizabeth O.\n%F AA(AAVSO)\n%J AAVSO Special Notice\n%V 429\n%D 05/2017\n%P 1\n%K astronomical databases: miscellaneous, binaries: symbiotic, stars:\nindividual (V694 Mon, MWC 560)\n%C (C) AAVSO 2017\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I Co-Reads: Co-Reads;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\n%B The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\n\n\n%R 2017sptz.prop13168Y\n%T Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\n%A Yan, Lin\n%J Spitzer Proposal\n%D 04/2017\n%P 13168\n%I ABSTRACT: Abstract;\n%I Spitzer: Spitzer Space Telescope;\n%U https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\n%B ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\n\n\n%R 2017MsT..........2A\n%T Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\n%A Azankpo, Severin\n%F AA(University of Stellenbosch)\n%J Masters Thesis\n%D 03/2017\n%P 2\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I PUB_HTML: Publisher Article;\n%I AUTHOR_PDF: Author PDF;\n%I PUB_PDF: Publisher PDF;\n%U https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\n%B The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\n\n\n%R 2016emo6.rept.....R\n%T The penumbral Moon\'s eclipse form 16 september 2016\n%A Rotaru, Adrian; Pteancu, Mircea; Zaharia, Cristian\n%F AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad,\nRomania), AC(Private Astronomical Observatory, Ploiesti, Romania)\n%J http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\n%D 10/2016\n%K THE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%U https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\n%B The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\n\n\n%R 2016iac..talk..872V\n%T Living on the edge: Adaptive Optics+Lucky Imaging\n%A Velasco, Sergio\n%F AA(Instituto de Astrofísica de Canarias)\n%J IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\n%D 03/2016\n%P 872\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I AUTHOR_HTML: Author Article;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\n%B Not Available

\n\n\n%R 2009bcet.book...65L\n%T The Diversity of Nuclear Magnetic Resonance Spectroscopy\n%A Liu, Corey W.; Alekseyev, Viktor Y.; Allwardt, Jeffrey R.; Bankovich,\nAlexander J.; Cade-Menun, Barbara J.; Davis, Ronald W.; Du, Lin-Shu;\nGarcia, K. Christopher; Herschlag, Daniel; Khosla, Chaitan; Kraut,\nDaniel A.; Li, Qing; Null, Brian; Puglisi, Joseph D.; Sigala, Paul A.;\nStebbins, Jonathan F.; Varani, Luca\n%F AA(Stanford Magnetic Resonance Laboratory, Stanford University),\nAB(Department of Chemistry, Stanford University; , Genencor),\nAC(Department of Geological & Environmental Sciences, Stanford\nUniversity; , ConocoPhillips Company), AD(Department of Molecular and\nCellular Physiology, Stanford University; Department of Structural\nBiology, Stanford University), AE(Department of Geological &\nEnvironmental Sciences, Stanford University; , Agriculture and Agri-Food\nCanada), AF(Stanford Genome Technology Center, Stanford University;\nDepartment of Biochemistry, Stanford University), AG(Department of\nGeological & Environmental Sciences, Stanford University; Air\nProducts and Chemicals, Inc. Allentown), AH(Department of Molecular and\nCellular Physiology, Stanford University; Department of Structural\nBiology, Stanford University), AI(Department of Biochemistry, Stanford\nUniversity), AJ(Department of Chemistry, Stanford University; Department\nof Biochemistry, Stanford University), AK(Department of Biochemistry,\nStanford University; Department of Biochemistry, Molecular Biology and\nCell Biology, Northwestern University), AL(Department of Chemistry,\nStanford University; , Institute for Research in Biomedicine),\nAM(Stanford Genome Technology Center, Stanford University; Department of\nBiochemistry, Stanford University), AN(Stanford Magnetic Resonance\nLaboratory, Stanford University; Department of Structural Biology,\nStanford University), AO(Department of Molecular and Cellular\nPhysiology, Stanford University; Department of Structural Biology,\nStanford University), AP(Department of Geological & Environmental\nSciences, Stanford University), AQ(Department of Molecular and Cellular\nPhysiology, Stanford University; Department of Structural Biology,\nStanford University)\n%J Biophysics and the Challenges of Emerging Threats\n%D 01/2009\n%P 65\n%K Physics\n%C (c) 2009: Springer Netherlands\n%I ABSTRACT: Abstract;\n%I TOC: Table of Contents;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\n%B The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\n%Y DOI: 10.1007/978-90-481-2368-1_5\n\n\n%R 2007AAS...210.2104M\n%T Time Domain Exploration with the Palomar-QUEST Sky Survey\n%A Mahabal, Ashish A.; Drake, A. J.; Djorgovski, S. G.; Donalek, C.;\nGlikman, E.; Graham, M. J.; Williams, R.; Baltay, C.; Rabinowitz, D.; PQ\nTeam Caltech; Yale; NCSA; Indiana; , . . .\n%F AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech),\nAF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\n%J American Astronomical Society Meeting Abstracts #210\n%V 210\n%D 05/2007\n%P 21.04\n%I ABSTRACT: Abstract;\n%I TOC: Table of Contents;\n%U https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\n%B Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\n\n\n%R 2007RJPh....1...35.\n%T Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n%A ., S. N. Agbo; ., E. C. Okoroigwe\n%J Research Journal of Physics\n%V 1\n%D 01/2007\n%P 35\n%L 41\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\n%B Not Available

\n%Y DOI: 10.3923/rjp.2007.35.41\n\n\n%R 1995ans..agar..390M\n%T Spacecraft navigation requirements\n%A Miller, Judy L.\n%F AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\n%J In AGARD\n%D 06/1995\n%P 390\n%L 405\n%K Earth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space\nNavigation, Spacecraft Trajectories, Support Systems, Technology\nAssessment, Technology Utilization, Ascent Trajectories, Reentry\nTrajectories, Spacecraft, Spacecraft Performance, Spacecraft\nSurvivability, Tradeoffs, Weight (Mass), Space Communications,\nSpacecraft Communications, Command and Tracking\n%I ABSTRACT: Abstract;\n%U https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\n%B Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\n\n\n%R 1995anda.book.....N\n%T Applied nonlinear dynamics: analytical, computational and experimental methods\n%A Nayfeh, Ali H.; Balachandran, Balakumar\n%J Wiley series in nonlinear science\n%D 01/1995\n%I ABSTRACT: Abstract;\n%I CITATIONS: Citations to the Article;\n%I Co-Reads: Co-Reads;\n%U https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\n%B Not Available

\n\n\n%R 1991hep.th....8028G\n%T Applied Conformal Field Theory\n%A Ginsparg, Paul\n%J arXiv e-prints\n%D 11/1988\n%P hep-th/9108028\n%K High Energy Physics - Theory\n%I ABSTRACT: Abstract;\n%I CITATIONS: Citations to the Article;\n%I Co-Reads: Co-Reads;\n%I EPRINT_HTML: arXiv Article;\n%I EPRINT_PDF: arXiv PDF;\n%U https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\n%B These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\n%Y eprintid: arXiv:hep-th/9108028\n\n\n%R 1983aiaa.meetY....K\n%T Autonomous navigation using lunar beacons\n%A Khatib, A. R.; Ellis, J.; French, J.; Null, G.; Yunck, T.; Wu, S.\n%F AA(California Institute of Technology, Jet Propulsion Laboratory,\nPasadena, CA), AB(California Institute of Technology, Jet Propulsion\nLaboratory, Pasadena, CA), AC(California Institute of Technology, Jet\nPropulsion Laboratory, Pasadena, CA), AD(California Institute of\nTechnology, Jet Propulsion Laboratory, Pasadena, CA), AE(California\nInstitute of Technology, Jet Propulsion Laboratory, Pasadena, CA),\nAF(California Institute of Technology, Jet Propulsion Laboratory,\nPasadena, CA)\n%J AIAA, Aerospace Sciences Meeting\n%D 01/1983\n%K Artificial Satellites, Autonomous Navigation, Earth-Moon System,\nLunar Communication, Radio Beacons, Radio Navigation, Space Navigation,\nDoppler Navigation, Least Squares Method, Orbit Calculation, Space\nCommunications, Spacecraft Communications, Command and Tracking\n%I ABSTRACT: Abstract;\n%U https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\n%B The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\n\n\n%R 2012ddsw.rept.....T\n%T Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\n%A Thornton, P. E.; Thornton, M. M.; Mayer, B. W.; Wilhelmi, N.; Wei,\nY.; Devarakonda, R.; Cook, R.\n%J Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\n%D 04/2012\n%K Daymet\n%C Oak Ridge National Laboratory\n%I ABSTRACT: Abstract;\n%I CITATIONS: Citations to the Article;\n%I Co-Reads: Co-Reads;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\n%B Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\n%Y DOI: 10.3334/ORNLDAAC/1219\n\n\n'} +data_ads = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '%R 2018Wthr...73Q..35.\n%T Book reviews\n%J Weather\n%V 73\n%D 01/2018\n%P 35\n%L 35\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\n%B Not Available

\n%Y DOI: 10.1002/wea.3072\n\n\n%R 2018TDM.....5a0201F\n%T 2D Materials: maintaining editorial quality\n%A Fal\'ko, Vladimir; Thomas, Ceri-Wyn\n%F AA(Editor in Chief, National Graphene Institute, University of\nManchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol,\nUnited Kingdom)\n%J 2D Materials\n%V 5\n%D 01/2018\n%P 010201\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\n%B Not Available

\n%Y DOI: 10.1088/2053-1583/aa9403\n\n\n%R 2018Spin....877001P\n%T Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\n%A Parkin, Stuart; Chantrell, Roy; Chang, Ching-Ray\n%J Spin\n%V 8\n%D 01/2018\n%P 1877001\n%C (c) 2018: World Scientific Publishing Company\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%I PUB_PDF: Publisher PDF;\n%U https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\n%B Not Available

\n%Y DOI: 10.1142/S2010324718770015\n\n\n%R 2018SAAS...38.....D\n%T Millimeter Astronomy\n%A Dessauges-Zavadsky, Miroslava; Pfenniger, Daniel\n%J Saas-Fee Advanced Course\n%V 38\n%D 01/2018\n%K Physics\n%C (c) 2018: Springer-Verlag GmbH Germany, part of Springer Nature\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%I TOC: Table of Contents;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\n%B Not Available

\n%Y DOI: 10.1007/978-3-662-57546-8\n\n\n%R 2018PhRvL.120b9901P\n%T Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\n%A Pustilnik, M.; van Heck, B.; Lutchyn, R. M.; Glazman, L. I.\n%J Physical Review Letters\n%V 120\n%D 01/2018\n%P 029901\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\n%B Not Available

\n%Y DOI: 10.1103/PhysRevLett.120.029901\n\n\n%R 2017PhDT........14C\n%T Resolving Gas-Phase Metallicity In Galaxies\n%A Carton, David\n%F AA(Leiden University)\n%J Ph.D. Thesis\n%D 06/2017\n%K galaxies: evolution, galaxies: abundances, galaxies: ISM\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\n%B Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\n%Y DOI: 10.5281/zenodo.581221\n\n\n%R 2017nova.pres.2388K\n%T A 3D View of a Supernova Remnant\n%A Kohler, Susanna\n%J AAS Nova Highlights\n%D 06/2017\n%P 2388\n%K Features, Highlights, interstellar medium, stellar evolution,\nsupernova remnant, supernovae, white dwarfs\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\n%B The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\n\n\n%R 2017CBET.4403....2G\n%T Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\n%A Green, D. W. E.\n%J Central Bureau Electronic Telegrams\n%V 4403\n%D 06/2017\n%P 2\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\n%B A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\n\n\n%R 2017ascl.soft06009C\n%T sick: Spectroscopic inference crank\n%A Casey, Andrew R.\n%J Astrophysics Source Code Library\n%D 06/2017\n%P ascl:1706.009\n%K Software\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\n%B sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\n%Y eprintid: ascl:1706.009\n\n\n%R 2017yCat.113380453S\n%T VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\n%A Siltala, J.; Jetsu, L.; Hackman, T.; Henry, G. W.; Immonen, L.;\nKajatkari, P.; Lankinen, J.; Lehtinen, J.; Monira, S.; Nikbakhsh, S.;\nViitanen, A.; Viuho, J.; Willamo, T.\n%J VizieR Online Data Catalog\n%D 05/2017\n%P J/AN/338/453\n%K Stars: variable\n%I ABSTRACT: Abstract;\n%I Vizier: VizieR Catalog Service;\n%U https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\n%X phot.dat 2930x19 Differential photometry of BM CVn; phot_mlc.dat 2930x19\nDifferential photometry of BM CVn with MLC removed; res.dat 1319x185\n*Numerical results of the CPS analysis; res_mlc.dat 1319x185 *Results of\nthe CPS analysis with MLC removed\n%B The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\n\n\n%R 2017AAVSN.429....1W\n%T V694 Mon (MWC 560) spectroscopy requested\n%A Waagen, Elizabeth O.\n%F AA(AAVSO)\n%J AAVSO Special Notice\n%V 429\n%D 05/2017\n%P 1\n%K astronomical databases: miscellaneous, binaries: symbiotic, stars:\nindividual (V694 Mon, MWC 560)\n%C (C) AAVSO 2017\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I Co-Reads: Co-Reads;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\n%B The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\n\n\n%R 2017sptz.prop13168Y\n%T Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\n%A Yan, Lin\n%J Spitzer Proposal\n%D 04/2017\n%P 13168\n%I ABSTRACT: Abstract;\n%I Spitzer: Spitzer Space Telescope;\n%U https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\n%B ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\n\n\n%R 2017MsT..........2A\n%T Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\n%A Azankpo, Severin\n%F AA(University of Stellenbosch)\n%J Masters Thesis\n%D 03/2017\n%P 2\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I PUB_HTML: Publisher Article;\n%I AUTHOR_PDF: Author PDF;\n%I PUB_PDF: Publisher PDF;\n%U https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\n%B The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\n\n\n%R 2016emo6.rept.....R\n%T The penumbral Moon\'s eclipse form 16 september 2016\n%A Rotaru, Adrian; Pteancu, Mircea; Zaharia, Cristian\n%F AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad,\nRomania), AC(Private Astronomical Observatory, Ploiesti, Romania)\n%J http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\n%D 10/2016\n%K THE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%U https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\n%B The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\n\n\n%R 2016iac..talk..872V\n%T Living on the edge: Adaptive Optics+Lucky Imaging\n%A Velasco, Sergio\n%F AA(Instituto de Astrofísica de Canarias)\n%J IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\n%D 03/2016\n%P 872\n%I ABSTRACT: Abstract;\n%I REFERENCES: References in the Article;\n%I AUTHOR_HTML: Author Article;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\n%B Not Available

\n\n\n%R 2009bcet.book...65L\n%T The Diversity of Nuclear Magnetic Resonance Spectroscopy\n%A Liu, Corey W.; Alekseyev, Viktor Y.; Allwardt, Jeffrey R.; Bankovich,\nAlexander J.; Cade-Menun, Barbara J.; Davis, Ronald W.; Du, Lin-Shu;\nGarcia, K. Christopher; Herschlag, Daniel; Khosla, Chaitan; Kraut,\nDaniel A.; Li, Qing; Null, Brian; Puglisi, Joseph D.; Sigala, Paul A.;\nStebbins, Jonathan F.; Varani, Luca\n%F AA(Stanford Magnetic Resonance Laboratory, Stanford University),\nAB(Department of Chemistry, Stanford University; , Genencor),\nAC(Department of Geological & Environmental Sciences, Stanford\nUniversity; , ConocoPhillips Company), AD(Department of Molecular and\nCellular Physiology, Stanford University; Department of Structural\nBiology, Stanford University), AE(Department of Geological &\nEnvironmental Sciences, Stanford University; , Agriculture and Agri-Food\nCanada), AF(Stanford Genome Technology Center, Stanford University;\nDepartment of Biochemistry, Stanford University), AG(Department of\nGeological & Environmental Sciences, Stanford University; Air\nProducts and Chemicals, Inc. Allentown), AH(Department of Molecular and\nCellular Physiology, Stanford University; Department of Structural\nBiology, Stanford University), AI(Department of Biochemistry, Stanford\nUniversity), AJ(Department of Chemistry, Stanford University; Department\nof Biochemistry, Stanford University), AK(Department of Biochemistry,\nStanford University; Department of Biochemistry, Molecular Biology and\nCell Biology, Northwestern University), AL(Department of Chemistry,\nStanford University; , Institute for Research in Biomedicine),\nAM(Stanford Genome Technology Center, Stanford University; Department of\nBiochemistry, Stanford University), AN(Stanford Magnetic Resonance\nLaboratory, Stanford University; Department of Structural Biology,\nStanford University), AO(Department of Molecular and Cellular\nPhysiology, Stanford University; Department of Structural Biology,\nStanford University), AP(Department of Geological & Environmental\nSciences, Stanford University), AQ(Department of Molecular and Cellular\nPhysiology, Stanford University; Department of Structural Biology,\nStanford University)\n%J Biophysics and the Challenges of Emerging Threats\n%D 01/2009\n%P 65\n%K Physics\n%C (c) 2009: Springer Netherlands\n%I ABSTRACT: Abstract;\n%I TOC: Table of Contents;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\n%B The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\n%Y DOI: 10.1007/978-90-481-2368-1_5\n\n\n%R 2007AAS...210.2104M\n%T Time Domain Exploration with the Palomar-QUEST Sky Survey\n%A Mahabal, Ashish A.; Drake, A. J.; Djorgovski, S. G.; Donalek, C.;\nGlikman, E.; Graham, M. J.; Williams, R.; Baltay, C.; Rabinowitz, D.; PQ\nTeam Caltech; Yale; NCSA; Indiana; , . . .\n%F AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech),\nAF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\n%J American Astronomical Society Meeting Abstracts #210\n%V 210\n%D 05/2007\n%P 21.04\n%I ABSTRACT: Abstract;\n%I TOC: Table of Contents;\n%U https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\n%B Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\n\n\n%R 2007RJPh....1...35.\n%T Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n%A ., S. N. Agbo; ., E. C. Okoroigwe\n%J Research Journal of Physics\n%V 1\n%D 01/2007\n%P 35\n%L 41\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\n%B Not Available

\n%Y DOI: 10.3923/rjp.2007.35.41\n\n\n%R 1995ans..agar..390M\n%T Spacecraft navigation requirements\n%A Miller, Judy L.\n%F AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\n%J In AGARD\n%D 06/1995\n%P 390\n%L 405\n%K Earth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space\nNavigation, Spacecraft Trajectories, Support Systems, Technology\nAssessment, Technology Utilization, Ascent Trajectories, Reentry\nTrajectories, Spacecraft, Spacecraft Performance, Spacecraft\nSurvivability, Tradeoffs, Weight (Mass), Space Communications,\nSpacecraft Communications, Command and Tracking\n%I ABSTRACT: Abstract;\n%U https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\n%B Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\n\n\n%R 1995anda.book.....N\n%T Applied nonlinear dynamics: analytical, computational and experimental methods\n%A Nayfeh, Ali H.; Balachandran, Balakumar\n%J Wiley series in nonlinear science\n%D 01/1995\n%I ABSTRACT: Abstract;\n%I CITATIONS: Citations to the Article;\n%I Co-Reads: Co-Reads;\n%U https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\n%B Not Available

\n\n\n%R 1991hep.th....8028G\n%T Applied Conformal Field Theory\n%A Ginsparg, Paul\n%J arXiv e-prints\n%D 11/1988\n%P hep-th/9108028\n%K High Energy Physics - Theory\n%I ABSTRACT: Abstract;\n%I CITATIONS: Citations to the Article;\n%I Co-Reads: Co-Reads;\n%I EPRINT_HTML: arXiv Article;\n%I EPRINT_PDF: arXiv PDF;\n%U https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\n%B These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\n%Y eprintid: arXiv:hep-th/9108028\n\n\n%R 1983aiaa.meetY....K\n%T Autonomous navigation using lunar beacons\n%A Khatib, A. R.; Ellis, J.; French, J.; Null, G.; Yunck, T.; Wu, S.\n%F AA(California Institute of Technology, Jet Propulsion Laboratory,\nPasadena, CA), AB(California Institute of Technology, Jet Propulsion\nLaboratory, Pasadena, CA), AC(California Institute of Technology, Jet\nPropulsion Laboratory, Pasadena, CA), AD(California Institute of\nTechnology, Jet Propulsion Laboratory, Pasadena, CA), AE(California\nInstitute of Technology, Jet Propulsion Laboratory, Pasadena, CA),\nAF(California Institute of Technology, Jet Propulsion Laboratory,\nPasadena, CA)\n%J AIAA, Aerospace Sciences Meeting\n%D 01/1983\n%K Artificial Satellites, Autonomous Navigation, Earth-Moon System,\nLunar Communication, Radio Beacons, Radio Navigation, Space Navigation,\nDoppler Navigation, Least Squares Method, Orbit Calculation, Space\nCommunications, Spacecraft Communications, Command and Tracking\n%I ABSTRACT: Abstract;\n%U https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\n%B The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\n\n\n%R 2012ddsw.rept.....T\n%T Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\n%A Thornton, P. E.; Thornton, M. M.; Mayer, B. W.; Wilhelmi, N.; Wei,\nY.; Devarakonda, R.; Cook, R.\n%J Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\n%D 04/2012\n%K Daymet\n%C Oak Ridge National Laboratory\n%I ABSTRACT: Abstract;\n%I CITATIONS: Citations to the Article;\n%I Co-Reads: Co-Reads;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\n%B Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\n%Y DOI: 10.3334/ORNLDAAC/1219\n\n\n%R 2020EPJC...80...96D\n%T Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\n%A Dhaygude, Akanksha; Desai, Shantanu\n%F AA(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana,\nIndia), AB(Department of Physics, IIT Hyderabad, 502285, Kandi,\nTelangana, India ;)\n%J European Physical Journal C\n%D 02/2020\n%K Astrophysics - High Energy Astrophysical Phenomena, Astrophysics -\nInstrumentation and Methods for Astrophysics, Nuclear Experiment\n%C © The Author(s) 2020\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%I EPRINT_HTML: arXiv Article;\n%I PUB_HTML: Publisher Article;\n%I EPRINT_PDF: arXiv PDF;\n%U https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\n%B Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\n%Y DOI: 10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\n%Y eprintid: arXiv:1912.06970\n\n\n'} -data_endnote= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '%0 Journal Article\n%T Book reviews\n%J Weather\n%V 73\n%D 2018\n%8 January 01, 2018\n%P 35-35\n%U https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\n%X Not Available

\n%R 10.1002/wea.3072\n%@ 0043-1656\n\n\n%0 Journal Article\n%T 2D Materials: maintaining editorial quality\n%A Fal\'ko, Vladimir\n%A Thomas, Ceri-Wyn\n%+ AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\n%J 2D Materials\n%V 5\n%D 2018\n%8 January 01, 2018\n%P 010201\n%U https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\n%X Not Available

\n%R 10.1088/2053-1583/aa9403\n%@ 2053-1583\n\n\n%0 Journal Article\n%T Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\n%A Parkin, Stuart\n%A Chantrell, Roy\n%A Chang, Ching-Ray\n%J Spin\n%V 8\n%D 2018\n%8 January 01, 2018\n%P 1877001\n%U https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\n%X Not Available

\n%R 10.1142/S2010324718770015\n\n\n%0 Journal Article\n%T Millimeter Astronomy\n%A Dessauges-Zavadsky, Miroslava\n%A Pfenniger, Daniel\n%J Saas-Fee Advanced Course\n%V 38\n%D 2018\n%8 January 01, 2018\n%K Physics\n%U https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\n%X Not Available

\n%R 10.1007/978-3-662-57546-8\n\n\n%0 Journal Article\n%T Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\n%A Pustilnik, M.\n%A van Heck, B.\n%A Lutchyn, R. M.\n%A Glazman, L. I.\n%J Physical Review Letters\n%V 120\n%D 2018\n%8 January 01, 2018\n%P 029901\n%U https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\n%X Not Available

\n%R 10.1103/PhysRevLett.120.029901\n%@ 0031-9007\n\n\n%0 Thesis\n%T Resolving Gas-Phase Metallicity In Galaxies\n%A Carton, David\n%+ AA(Leiden University)\n%J Ph.D. Thesis\n%D 2017\n%8 June 01, 2017\n%K galaxies: evolution; galaxies: abundances; galaxies: ISM\n%U https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\n%X Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\n%R 10.5281/zenodo.581221\n\n\n%0 Journal Article\n%T A 3D View of a Supernova Remnant\n%A Kohler, Susanna\n%J AAS Nova Highlights\n%D 2017\n%8 June 01, 2017\n%P 2388\n%K Features; Highlights; interstellar medium; stellar evolution;\nsupernova remnant; supernovae; white dwarfs\n%U https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\n%X The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\n\n\n%0 Journal Article\n%T Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\n%A Green, D. W. E.\n%J Central Bureau Electronic Telegrams\n%V 4403\n%D 2017\n%8 June 01, 2017\n%P 2\n%U https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\n%X A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\n\n\n%0 Miscellaneous\n%T sick: Spectroscopic inference crank\n%A Casey, Andrew R.\n%J Astrophysics Source Code Library\n%D 2017\n%8 June 01, 2017\n%P ascl:1706.009\n%K Software\n%U https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\n%X sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\n%= eprint: ascl:1706.009\n\n\n%0 Journal Article\n%T VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\n%A Siltala, J.\n%A Jetsu, L.\n%A Hackman, T.\n%A Henry, G. W.\n%A Immonen, L.\n%A Kajatkari, P.\n%A Lankinen, J.\n%A Lehtinen, J.\n%A Monira, S.\n%A Nikbakhsh, S.\n%A Viitanen, A.\n%A Viuho, J.\n%A Willamo, T.\n%J VizieR Online Data Catalog\n%D 2017\n%8 May 01, 2017\n%P J/AN/338/453\n%K Stars: variable\n%U https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\n%Z phot.dat 2930x19 Differential photometry of BM CVn; phot_mlc.dat 2930x19\nDifferential photometry of BM CVn with MLC removed; res.dat 1319x185\n*Numerical results of the CPS analysis; res_mlc.dat 1319x185 *Results of\nthe CPS analysis with MLC removed\n%X The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\n\n\n%0 Journal Article\n%T V694 Mon (MWC 560) spectroscopy requested\n%A Waagen, Elizabeth O.\n%+ AA(AAVSO)\n%J AAVSO Special Notice\n%V 429\n%D 2017\n%8 May 01, 2017\n%P 1\n%K astronomical databases: miscellaneous; binaries: symbiotic; stars:\nindividual (V694 Mon; MWC 560)\n%U https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\n%X The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\n\n\n%0 Miscellaneous\n%T Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\n%A Yan, Lin\n%J Spitzer Proposal\n%D 2017\n%8 April 01, 2017\n%P 13168\n%U https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\n%X ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\n\n\n%0 Thesis\n%T Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\n%A Azankpo, Severin\n%+ AA(University of Stellenbosch)\n%J Masters Thesis\n%D 2017\n%8 March 01, 2017\n%P 2\n%U https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\n%X The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\n\n\n%0 Report\n%T The penumbral Moon\'s eclipse form 16 september 2016\n%A Rotaru, Adrian\n%A Pteancu, Mircea\n%A Zaharia, Cristian\n%+ AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\n%J http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\n%D 2016\n%8 October 01, 2016\n%K THE MOON; ECLIPSES; PARTIAL; PENUMBRAL; ASTROPHOTOGRAPHY\n%U https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\n%X The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\n\n\n%0 Conference Paper\n%T Living on the edge: Adaptive Optics+Lucky Imaging\n%A Velasco, Sergio\n%+ AA(Instituto de Astrofísica de Canarias)\n%J IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\n%D 2016\n%8 March 01, 2016\n%P 872\n%U https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\n%X Not Available

\n\n\n%0 Book Section\n%T The Diversity of Nuclear Magnetic Resonance Spectroscopy\n%A Liu, Corey W.\n%A Alekseyev, Viktor Y.\n%A Allwardt, Jeffrey R.\n%A Bankovich, Alexander J.\n%A Cade-Menun, Barbara J.\n%A Davis, Ronald W.\n%A Du, Lin-Shu\n%A Garcia, K. Christopher\n%A Herschlag, Daniel\n%A Khosla, Chaitan\n%A Kraut, Daniel A.\n%A Li, Qing\n%A Null, Brian\n%A Puglisi, Joseph D.\n%A Sigala, Paul A.\n%A Stebbins, Jonathan F.\n%A Varani, Luca\n%E Puglisi, Joseph D.\n%+ AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\n%B Biophysics and the Challenges of Emerging Threats\n%D 2009\n%8 January 01, 2009\n%P 65\n%K Physics\n%U https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\n%X The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\n%R 10.1007/978-90-481-2368-1_5\n\n\n%0 Conference Paper\n%T Time Domain Exploration with the Palomar-QUEST Sky Survey\n%A Mahabal, Ashish A.\n%A Drake, A. J.\n%A Djorgovski, S. G.\n%A Donalek, C.\n%A Glikman, E.\n%A Graham, M. J.\n%A Williams, R.\n%A Baltay, C.\n%A Rabinowitz, D.\n%A PQ Team Caltech\n%A Yale\n%A NCSA\n%A Indiana\n%A , . . .\n%+ AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\n%B American Astronomical Society Meeting Abstracts #210\n%V 210\n%D 2007\n%8 May 01, 2007\n%P 21.04\n%U https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\n%X Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\n\n\n%0 Journal Article\n%T Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n%A ., S. N. Agbo\n%A ., E. C. Okoroigwe\n%J Research Journal of Physics\n%V 1\n%D 2007\n%8 January 01, 2007\n%P 35-41\n%U https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\n%X Not Available

\n%R 10.3923/rjp.2007.35.41\n%@ 1819-3463\n\n\n%0 Conference Proceedings\n%T Spacecraft navigation requirements\n%A Miller, Judy L.\n%+ AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\n%B In AGARD\n%D 1995\n%8 June 01, 1995\n%P 390-405\n%K Earth Orbits; Navigation Aids; Navigators; Onboard Equipment; Space\nNavigation; Spacecraft Trajectories; Support Systems; Technology\nAssessment; Technology Utilization; Ascent Trajectories; Reentry\nTrajectories; Spacecraft; Spacecraft Performance; Spacecraft\nSurvivability; Tradeoffs; Weight (Mass); Space Communications,\nSpacecraft Communications, Command and Tracking\n%U https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\n%X Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\n\n\n%0 Book\n%T Applied nonlinear dynamics: analytical, computational and experimental methods\n%A Nayfeh, Ali H.\n%A Balachandran, Balakumar\n%J Wiley series in nonlinear science\n%D 1995\n%8 January 01, 1995\n%U https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\n%X Not Available

\n\n\n%0 Electronic Article\n%T Applied Conformal Field Theory\n%A Ginsparg, Paul\n%J arXiv e-prints\n%D 1988\n%8 November 01, 1988\n%P hep-th/9108028\n%K High Energy Physics - Theory\n%U https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\n%X These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\n%= eprint: arXiv:hep-th/9108028\n\n\n%0 Conference Proceedings\n%T Autonomous navigation using lunar beacons\n%A Khatib, A. R.\n%A Ellis, J.\n%A French, J.\n%A Null, G.\n%A Yunck, T.\n%A Wu, S.\n%+ AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\n%B AIAA, Aerospace Sciences Meeting\n%C Reno, NV\n%D 1983\n%8 January 01, 1983\n%K Artificial Satellites; Autonomous Navigation; Earth-Moon System;\nLunar Communication; Radio Beacons; Radio Navigation; Space Navigation;\nDoppler Navigation; Least Squares Method; Orbit Calculation; Space\nCommunications, Spacecraft Communications, Command and Tracking\n%U https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\n%X The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\n\n\n%0 Miscellaneous\n%T Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\n%A Thornton, P. E.\n%A Thornton, M. M.\n%A Mayer, B. W.\n%A Wilhelmi, N.\n%A Wei, Y.\n%A Devarakonda, R.\n%A Cook, R.\n%J Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\n%D 2012\n%8 April 01, 2012\n%K Daymet\n%U https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\n%X Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\n%R 10.3334/ORNLDAAC/1219\n\n\n'} +data_endnote= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '%0 Journal Article\n%T Book reviews\n%J Weather\n%V 73\n%D 2018\n%8 January 01, 2018\n%P 35-35\n%U https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\n%X Not Available

\n%R 10.1002/wea.3072\n%@ 0043-1656\n\n\n%0 Journal Article\n%T 2D Materials: maintaining editorial quality\n%A Fal\'ko, Vladimir\n%A Thomas, Ceri-Wyn\n%+ AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\n%J 2D Materials\n%V 5\n%D 2018\n%8 January 01, 2018\n%P 010201\n%U https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\n%X Not Available

\n%R 10.1088/2053-1583/aa9403\n%@ 2053-1583\n\n\n%0 Journal Article\n%T Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\n%A Parkin, Stuart\n%A Chantrell, Roy\n%A Chang, Ching-Ray\n%J Spin\n%V 8\n%D 2018\n%8 January 01, 2018\n%P 1877001\n%U https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\n%X Not Available

\n%R 10.1142/S2010324718770015\n\n\n%0 Journal Article\n%T Millimeter Astronomy\n%A Dessauges-Zavadsky, Miroslava\n%A Pfenniger, Daniel\n%J Saas-Fee Advanced Course\n%V 38\n%D 2018\n%8 January 01, 2018\n%K Physics\n%U https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\n%X Not Available

\n%R 10.1007/978-3-662-57546-8\n\n\n%0 Journal Article\n%T Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\n%A Pustilnik, M.\n%A van Heck, B.\n%A Lutchyn, R. M.\n%A Glazman, L. I.\n%J Physical Review Letters\n%V 120\n%D 2018\n%8 January 01, 2018\n%P 029901\n%U https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\n%X Not Available

\n%R 10.1103/PhysRevLett.120.029901\n%@ 0031-9007\n\n\n%0 Thesis\n%T Resolving Gas-Phase Metallicity In Galaxies\n%A Carton, David\n%+ AA(Leiden University)\n%J Ph.D. Thesis\n%D 2017\n%8 June 01, 2017\n%K galaxies: evolution; galaxies: abundances; galaxies: ISM\n%U https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\n%X Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\n%R 10.5281/zenodo.581221\n\n\n%0 Journal Article\n%T A 3D View of a Supernova Remnant\n%A Kohler, Susanna\n%J AAS Nova Highlights\n%D 2017\n%8 June 01, 2017\n%P 2388\n%K Features; Highlights; interstellar medium; stellar evolution;\nsupernova remnant; supernovae; white dwarfs\n%U https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\n%X The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\n\n\n%0 Journal Article\n%T Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\n%A Green, D. W. E.\n%J Central Bureau Electronic Telegrams\n%V 4403\n%D 2017\n%8 June 01, 2017\n%P 2\n%U https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\n%X A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\n\n\n%0 Miscellaneous\n%T sick: Spectroscopic inference crank\n%A Casey, Andrew R.\n%J Astrophysics Source Code Library\n%D 2017\n%8 June 01, 2017\n%P ascl:1706.009\n%K Software\n%U https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\n%X sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\n%= eprint: ascl:1706.009\n\n\n%0 Journal Article\n%T VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\n%A Siltala, J.\n%A Jetsu, L.\n%A Hackman, T.\n%A Henry, G. W.\n%A Immonen, L.\n%A Kajatkari, P.\n%A Lankinen, J.\n%A Lehtinen, J.\n%A Monira, S.\n%A Nikbakhsh, S.\n%A Viitanen, A.\n%A Viuho, J.\n%A Willamo, T.\n%J VizieR Online Data Catalog\n%D 2017\n%8 May 01, 2017\n%P J/AN/338/453\n%K Stars: variable\n%U https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\n%Z phot.dat 2930x19 Differential photometry of BM CVn; phot_mlc.dat 2930x19\nDifferential photometry of BM CVn with MLC removed; res.dat 1319x185\n*Numerical results of the CPS analysis; res_mlc.dat 1319x185 *Results of\nthe CPS analysis with MLC removed\n%X The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\n\n\n%0 Journal Article\n%T V694 Mon (MWC 560) spectroscopy requested\n%A Waagen, Elizabeth O.\n%+ AA(AAVSO)\n%J AAVSO Special Notice\n%V 429\n%D 2017\n%8 May 01, 2017\n%P 1\n%K astronomical databases: miscellaneous; binaries: symbiotic; stars:\nindividual (V694 Mon; MWC 560)\n%U https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\n%X The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\n\n\n%0 Miscellaneous\n%T Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\n%A Yan, Lin\n%J Spitzer Proposal\n%D 2017\n%8 April 01, 2017\n%P 13168\n%U https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\n%X ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\n\n\n%0 Thesis\n%T Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\n%A Azankpo, Severin\n%+ AA(University of Stellenbosch)\n%J Masters Thesis\n%D 2017\n%8 March 01, 2017\n%P 2\n%U https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\n%X The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\n\n\n%0 Report\n%T The penumbral Moon\'s eclipse form 16 september 2016\n%A Rotaru, Adrian\n%A Pteancu, Mircea\n%A Zaharia, Cristian\n%+ AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\n%J http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\n%D 2016\n%8 October 01, 2016\n%K THE MOON; ECLIPSES; PARTIAL; PENUMBRAL; ASTROPHOTOGRAPHY\n%U https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\n%X The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\n\n\n%0 Conference Paper\n%T Living on the edge: Adaptive Optics+Lucky Imaging\n%A Velasco, Sergio\n%+ AA(Instituto de Astrofísica de Canarias)\n%J IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\n%D 2016\n%8 March 01, 2016\n%P 872\n%U https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\n%X Not Available

\n\n\n%0 Book Section\n%T The Diversity of Nuclear Magnetic Resonance Spectroscopy\n%A Liu, Corey W.\n%A Alekseyev, Viktor Y.\n%A Allwardt, Jeffrey R.\n%A Bankovich, Alexander J.\n%A Cade-Menun, Barbara J.\n%A Davis, Ronald W.\n%A Du, Lin-Shu\n%A Garcia, K. Christopher\n%A Herschlag, Daniel\n%A Khosla, Chaitan\n%A Kraut, Daniel A.\n%A Li, Qing\n%A Null, Brian\n%A Puglisi, Joseph D.\n%A Sigala, Paul A.\n%A Stebbins, Jonathan F.\n%A Varani, Luca\n%E Puglisi, Joseph D.\n%+ AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\n%B Biophysics and the Challenges of Emerging Threats\n%D 2009\n%8 January 01, 2009\n%P 65\n%K Physics\n%U https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\n%X The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\n%R 10.1007/978-90-481-2368-1_5\n\n\n%0 Conference Paper\n%T Time Domain Exploration with the Palomar-QUEST Sky Survey\n%A Mahabal, Ashish A.\n%A Drake, A. J.\n%A Djorgovski, S. G.\n%A Donalek, C.\n%A Glikman, E.\n%A Graham, M. J.\n%A Williams, R.\n%A Baltay, C.\n%A Rabinowitz, D.\n%A PQ Team Caltech\n%A Yale\n%A NCSA\n%A Indiana\n%A , . . .\n%+ AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\n%B American Astronomical Society Meeting Abstracts #210\n%V 210\n%D 2007\n%8 May 01, 2007\n%P 21.04\n%U https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\n%X Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\n\n\n%0 Journal Article\n%T Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n%A ., S. N. Agbo\n%A ., E. C. Okoroigwe\n%J Research Journal of Physics\n%V 1\n%D 2007\n%8 January 01, 2007\n%P 35-41\n%U https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\n%X Not Available

\n%R 10.3923/rjp.2007.35.41\n%@ 1819-3463\n\n\n%0 Conference Proceedings\n%T Spacecraft navigation requirements\n%A Miller, Judy L.\n%+ AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\n%B In AGARD\n%D 1995\n%8 June 01, 1995\n%P 390-405\n%K Earth Orbits; Navigation Aids; Navigators; Onboard Equipment; Space\nNavigation; Spacecraft Trajectories; Support Systems; Technology\nAssessment; Technology Utilization; Ascent Trajectories; Reentry\nTrajectories; Spacecraft; Spacecraft Performance; Spacecraft\nSurvivability; Tradeoffs; Weight (Mass); Space Communications,\nSpacecraft Communications, Command and Tracking\n%U https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\n%X Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\n\n\n%0 Book\n%T Applied nonlinear dynamics: analytical, computational and experimental methods\n%A Nayfeh, Ali H.\n%A Balachandran, Balakumar\n%J Wiley series in nonlinear science\n%D 1995\n%8 January 01, 1995\n%U https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\n%X Not Available

\n\n\n%0 Electronic Article\n%T Applied Conformal Field Theory\n%A Ginsparg, Paul\n%J arXiv e-prints\n%D 1988\n%8 November 01, 1988\n%P hep-th/9108028\n%K High Energy Physics - Theory\n%U https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\n%X These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\n%= eprint: arXiv:hep-th/9108028\n\n\n%0 Conference Proceedings\n%T Autonomous navigation using lunar beacons\n%A Khatib, A. R.\n%A Ellis, J.\n%A French, J.\n%A Null, G.\n%A Yunck, T.\n%A Wu, S.\n%+ AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\n%B AIAA, Aerospace Sciences Meeting\n%C Reno, NV\n%D 1983\n%8 January 01, 1983\n%K Artificial Satellites; Autonomous Navigation; Earth-Moon System;\nLunar Communication; Radio Beacons; Radio Navigation; Space Navigation;\nDoppler Navigation; Least Squares Method; Orbit Calculation; Space\nCommunications, Spacecraft Communications, Command and Tracking\n%U https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\n%X The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\n\n\n%0 Miscellaneous\n%T Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\n%A Thornton, P. E.\n%A Thornton, M. M.\n%A Mayer, B. W.\n%A Wilhelmi, N.\n%A Wei, Y.\n%A Devarakonda, R.\n%A Cook, R.\n%J Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\n%D 2012\n%8 April 01, 2012\n%K Daymet\n%U https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\n%X Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\n%R 10.3334/ORNLDAAC/1219\n\n\n%0 Journal Article\n%T Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\n%A Dhaygude, Akanksha\n%A Desai, Shantanu\n%+ AA(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India), AB(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India ;)\n%J European Physical Journal C\n%D 2020\n%8 February 01, 2020\n%K Astrophysics - High Energy Astrophysical Phenomena; Astrophysics -\nInstrumentation and Methods for Astrophysics; Nuclear Experiment\n%U https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\n%X Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\n%R 10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\n%= eprint: arXiv:1912.06970\n\n\n'} -data_procite= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': u'TY - Journal\nTI - Book reviews\nJO - Weather\nVL - 73\nY1 - 2018/01/1\nSP - 35\nEP - 35\nUR - https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nN2 - Not Available

\nDO - 10.1002/wea.3072\nSN - 0043-1656\nER -\n\n\nTY - Journal\nTI - 2D Materials: maintaining editorial quality\nAU - Fal\'ko, Vladimir\nAU - Thomas, Ceri-Wyn\nAD - AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\nJO - 2D Materials\nVL - 5\nY1 - 2018/01/1\nSP - 010201\nUR - https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nN2 - Not Available

\nDO - 10.1088/2053-1583/aa9403\nSN - 2053-1583\nER -\n\n\nTY - Journal\nTI - Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nAU - Parkin, Stuart\nAU - Chantrell, Roy\nAU - Chang, Ching-Ray\nJO - Spin\nVL - 8\nY1 - 2018/01/1\nSP - 1877001\nUR - https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nN2 - Not Available

\nDO - 10.1142/S2010324718770015\nER -\n\n\nTY - Journal\nTI - Millimeter Astronomy\nAU - Dessauges-Zavadsky, Miroslava\nAU - Pfenniger, Daniel\nJO - Saas-Fee Advanced Course\nVL - 38\nY1 - 2018/01/1\nKW - Physics\nUR - https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nN2 - Not Available

\nDO - 10.1007/978-3-662-57546-8\nER -\n\n\nTY - Journal\nTI - Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nAU - Pustilnik, M.\nAU - van Heck, B.\nAU - Lutchyn, R. M.\nAU - Glazman, L. I.\nJO - Physical Review Letters\nVL - 120\nY1 - 2018/01/1\nSP - 029901\nUR - https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nN2 - Not Available

\nDO - 10.1103/PhysRevLett.120.029901\nSN - 0031-9007\nER -\n\n\nTY - Thesis/Dissertation\nTI - Resolving Gas-Phase Metallicity In Galaxies\nAU - Carton, David\nAD - AA(Leiden University)\nJO - Ph.D. Thesis\nY1 - 2017/06/1\nKW - galaxies: evolution/ galaxies: abundances/ galaxies: ISM\nUR - https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nN2 - Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\nDO - 10.5281/zenodo.581221\nER -\n\n\nTY - Journal\nTI - A 3D View of a Supernova Remnant\nAU - Kohler, Susanna\nJO - AAS Nova Highlights\nY1 - 2017/06/1\nSP - 2388\nKW - Features/ Highlights/ interstellar medium/ stellar evolution/\nsupernova remnant/ supernovae/ white dwarfs\nUR - https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nN2 - The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\nER -\n\n\nTY - Journal\nTI - Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nAU - Green, D. W. E.\nJO - Central Bureau Electronic Telegrams\nVL - 4403\nY1 - 2017/06/1\nSP - 2\nUR - https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nN2 - A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\nER -\n\n\nTY - Miscellaneous\nTI - sick: Spectroscopic inference crank\nAU - Casey, Andrew R.\nJO - Astrophysics Source Code Library\nY1 - 2017/06/1\nSP - ascl:1706.009\nKW - Software\nUR - https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nN2 - sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\nC1 - eprint: ascl:1706.009\nER -\n\n\nTY - Journal\nTI - VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nAU - Siltala, J.\nAU - Jetsu, L.\nAU - Hackman, T.\nAU - Henry, G. W.\nAU - Immonen, L.\nAU - Kajatkari, P.\nAU - Lankinen, J.\nAU - Lehtinen, J.\nAU - Monira, S.\nAU - Nikbakhsh, S.\nAU - Viitanen, A.\nAU - Viuho, J.\nAU - Willamo, T.\nJO - VizieR Online Data Catalog\nY1 - 2017/05/1\nSP - J/AN/338/453\nKW - Stars: variable\nUR - https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nN2 - The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\nER -\n\n\nTY - Journal\nTI - V694 Mon (MWC 560) spectroscopy requested\nAU - Waagen, Elizabeth O.\nAD - AA(AAVSO)\nJO - AAVSO Special Notice\nVL - 429\nY1 - 2017/05/1\nSP - 1\nKW - astronomical databases: miscellaneous/ binaries: symbiotic/ stars:\nindividual (V694 Mon/ MWC 560)\nUR - https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nN2 - The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi P\xe9ter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\nER -\n\n\nTY - Miscellaneous\nTI - Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nAU - Yan, Lin\nJO - Spitzer Proposal\nY1 - 2017/04/1\nSP - 13168\nUR - https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nN2 - ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\nER -\n\n\nTY - Thesis/Dissertation\nTI - Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAU - Azankpo, Severin\nAD - AA(University of Stellenbosch)\nJO - Masters Thesis\nY1 - 2017/03/1\nSP - 2\nUR - https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nN2 - The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\nER -\n\n\nTY - Report\nTI - The penumbral Moon\'s eclipse form 16 september 2016\nAU - Rotaru, Adrian\nAU - Pteancu, Mircea\nAU - Zaharia, Cristian\nAD - AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nJO - http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\nY1 - 2016/10/1\nKW - THE MOON/ ECLIPSES/ PARTIAL/ PENUMBRAL/ ASTROPHOTOGRAPHY\nUR - https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nN2 - The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\nER -\n\n\nTY - Conference\nTI - Living on the edge: Adaptive Optics+Lucky Imaging\nAU - Velasco, Sergio\nAD - AA(Instituto de Astrof\xedsica de Canarias)\nJO - IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\nY1 - 2016/03/1\nSP - 872\nUR - https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nN2 - Not Available

\nER -\n\n\nTY - Book Chapter\nTI - The Diversity of Nuclear Magnetic Resonance Spectroscopy\nAU - Liu, Corey W.\nAU - Alekseyev, Viktor Y.\nAU - Allwardt, Jeffrey R.\nAU - Bankovich, Alexander J.\nAU - Cade-Menun, Barbara J.\nAU - Davis, Ronald W.\nAU - Du, Lin-Shu\nAU - Garcia, K. Christopher\nAU - Herschlag, Daniel\nAU - Khosla, Chaitan\nAU - Kraut, Daniel A.\nAU - Li, Qing\nAU - Null, Brian\nAU - Puglisi, Joseph D.\nAU - Sigala, Paul A.\nAU - Stebbins, Jonathan F.\nAU - Varani, Luca\nAD - AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nJO - Biophysics and the Challenges of Emerging Threats\nY1 - 2009/01/1\nSP - 65\nKW - Physics\nUR - https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nN2 - The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\nDO - 10.1007/978-90-481-2368-1_5\nER -\n\n\nTY - Conference\nTI - Time Domain Exploration with the Palomar-QUEST Sky Survey\nAU - Mahabal, Ashish A.\nAU - Drake, A. J.\nAU - Djorgovski, S. G.\nAU - Donalek, C.\nAU - Glikman, E.\nAU - Graham, M. J.\nAU - Williams, R.\nAU - Baltay, C.\nAU - Rabinowitz, D.\nAU - PQ Team Caltech\nAU - Yale\nAU - NCSA\nAU - Indiana\nAU - , . . .\nAD - AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nJO - American Astronomical Society Meeting Abstracts #210\nVL - 210\nY1 - 2007/05/1\nSP - 21.04\nUR - https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nN2 - Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\nER -\n\n\nTY - Journal\nTI - Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nAU - ., S. N. Agbo\nAU - ., E. C. Okoroigwe\nJO - Research Journal of Physics\nVL - 1\nY1 - 2007/01/1\nSP - 35\nEP - 41\nUR - https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nN2 - Not Available

\nDO - 10.3923/rjp.2007.35.41\nSN - 1819-3463\nER -\n\n\nTY - Conference\nTI - Spacecraft navigation requirements\nAU - Miller, Judy L.\nAD - AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nJO - In AGARD\nY1 - 1995/06/1\nSP - 390\nEP - 405\nKW - Earth Orbits/ Navigation Aids/ Navigators/ Onboard Equipment/\nSpace Navigation/ Spacecraft Trajectories/ Support Systems/ Technology\nAssessment/ Technology Utilization/ Ascent Trajectories/ Reentry\nTrajectories/ Spacecraft/ Spacecraft Performance/ Spacecraft\nSurvivability/ Tradeoffs/ Weight (Mass)/ Space Communications,\nSpacecraft Communications, Command and Tracking\nUR - https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nN2 - Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\nER -\n\n\nTY - Book, Whole\nTI - Applied nonlinear dynamics: analytical, computational and experimental methods\nAU - Nayfeh, Ali H.\nAU - Balachandran, Balakumar\nJO - Wiley series in nonlinear science\nY1 - 1995/01/1\nUR - https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nN2 - Not Available

\nER -\n\n\nTY - Preprint\nTI - Applied Conformal Field Theory\nAU - Ginsparg, Paul\nJO - arXiv e-prints\nY1 - 1988/11/1\nSP - hep-th/9108028\nKW - High Energy Physics - Theory\nUR - https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nN2 - These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\nC1 - eprint: arXiv:hep-th/9108028\nER -\n\n\nTY - Journal\nTI - Autonomous navigation using lunar beacons\nAU - Khatib, A. R.\nAU - Ellis, J.\nAU - French, J.\nAU - Null, G.\nAU - Yunck, T.\nAU - Wu, S.\nAD - AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nJO - AIAA, Aerospace Sciences Meeting\nY1 - 1983/01/1\nKW - Artificial Satellites/ Autonomous Navigation/ Earth-Moon System/\nLunar Communication/ Radio Beacons/ Radio Navigation/ Space Navigation/\nDoppler Navigation/ Least Squares Method/ Orbit Calculation/ Space\nCommunications, Spacecraft Communications, Command and Tracking\nUR - https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nN2 - The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\nER -\n\n\nTY - Miscellaneous\nTI - Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nAU - Thornton, P. E.\nAU - Thornton, M. M.\nAU - Mayer, B. W.\nAU - Wilhelmi, N.\nAU - Wei, Y.\nAU - Devarakonda, R.\nAU - Cook, R.\nJO - Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\nY1 - 2012/04/1\nKW - Daymet\nUR - https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nN2 - Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\nDO - 10.3334/ORNLDAAC/1219\nER -\n\n\n'} +data_procite= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': u'TY - Journal\nTI - Book reviews\nJO - Weather\nVL - 73\nY1 - 2018/01/1\nSP - 35\nEP - 35\nUR - https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nN2 - Not Available

\nDO - 10.1002/wea.3072\nSN - 0043-1656\nER -\n\n\nTY - Journal\nTI - 2D Materials: maintaining editorial quality\nAU - Fal\'ko, Vladimir\nAU - Thomas, Ceri-Wyn\nAD - AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\nJO - 2D Materials\nVL - 5\nY1 - 2018/01/1\nSP - 010201\nUR - https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nN2 - Not Available

\nDO - 10.1088/2053-1583/aa9403\nSN - 2053-1583\nER -\n\n\nTY - Journal\nTI - Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nAU - Parkin, Stuart\nAU - Chantrell, Roy\nAU - Chang, Ching-Ray\nJO - Spin\nVL - 8\nY1 - 2018/01/1\nSP - 1877001\nUR - https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nN2 - Not Available

\nDO - 10.1142/S2010324718770015\nER -\n\n\nTY - Journal\nTI - Millimeter Astronomy\nAU - Dessauges-Zavadsky, Miroslava\nAU - Pfenniger, Daniel\nJO - Saas-Fee Advanced Course\nVL - 38\nY1 - 2018/01/1\nKW - Physics\nUR - https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nN2 - Not Available

\nDO - 10.1007/978-3-662-57546-8\nER -\n\n\nTY - Journal\nTI - Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nAU - Pustilnik, M.\nAU - van Heck, B.\nAU - Lutchyn, R. M.\nAU - Glazman, L. I.\nJO - Physical Review Letters\nVL - 120\nY1 - 2018/01/1\nSP - 029901\nUR - https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nN2 - Not Available

\nDO - 10.1103/PhysRevLett.120.029901\nSN - 0031-9007\nER -\n\n\nTY - Thesis/Dissertation\nTI - Resolving Gas-Phase Metallicity In Galaxies\nAU - Carton, David\nAD - AA(Leiden University)\nJO - Ph.D. Thesis\nY1 - 2017/06/1\nKW - galaxies: evolution/ galaxies: abundances/ galaxies: ISM\nUR - https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nN2 - Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\nDO - 10.5281/zenodo.581221\nER -\n\n\nTY - Journal\nTI - A 3D View of a Supernova Remnant\nAU - Kohler, Susanna\nJO - AAS Nova Highlights\nY1 - 2017/06/1\nSP - 2388\nKW - Features/ Highlights/ interstellar medium/ stellar evolution/\nsupernova remnant/ supernovae/ white dwarfs\nUR - https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nN2 - The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\nER -\n\n\nTY - Journal\nTI - Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nAU - Green, D. W. E.\nJO - Central Bureau Electronic Telegrams\nVL - 4403\nY1 - 2017/06/1\nSP - 2\nUR - https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nN2 - A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\nER -\n\n\nTY - Miscellaneous\nTI - sick: Spectroscopic inference crank\nAU - Casey, Andrew R.\nJO - Astrophysics Source Code Library\nY1 - 2017/06/1\nSP - ascl:1706.009\nKW - Software\nUR - https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nN2 - sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\nC1 - eprint: ascl:1706.009\nER -\n\n\nTY - Journal\nTI - VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nAU - Siltala, J.\nAU - Jetsu, L.\nAU - Hackman, T.\nAU - Henry, G. W.\nAU - Immonen, L.\nAU - Kajatkari, P.\nAU - Lankinen, J.\nAU - Lehtinen, J.\nAU - Monira, S.\nAU - Nikbakhsh, S.\nAU - Viitanen, A.\nAU - Viuho, J.\nAU - Willamo, T.\nJO - VizieR Online Data Catalog\nY1 - 2017/05/1\nSP - J/AN/338/453\nKW - Stars: variable\nUR - https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nN2 - The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\nER -\n\n\nTY - Journal\nTI - V694 Mon (MWC 560) spectroscopy requested\nAU - Waagen, Elizabeth O.\nAD - AA(AAVSO)\nJO - AAVSO Special Notice\nVL - 429\nY1 - 2017/05/1\nSP - 1\nKW - astronomical databases: miscellaneous/ binaries: symbiotic/ stars:\nindividual (V694 Mon/ MWC 560)\nUR - https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nN2 - The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi P\xe9ter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\nER -\n\n\nTY - Miscellaneous\nTI - Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nAU - Yan, Lin\nJO - Spitzer Proposal\nY1 - 2017/04/1\nSP - 13168\nUR - https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nN2 - ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\nER -\n\n\nTY - Thesis/Dissertation\nTI - Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAU - Azankpo, Severin\nAD - AA(University of Stellenbosch)\nJO - Masters Thesis\nY1 - 2017/03/1\nSP - 2\nUR - https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nN2 - The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\nER -\n\n\nTY - Report\nTI - The penumbral Moon\'s eclipse form 16 september 2016\nAU - Rotaru, Adrian\nAU - Pteancu, Mircea\nAU - Zaharia, Cristian\nAD - AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nJO - http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\nY1 - 2016/10/1\nKW - THE MOON/ ECLIPSES/ PARTIAL/ PENUMBRAL/ ASTROPHOTOGRAPHY\nUR - https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nN2 - The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\nER -\n\n\nTY - Conference\nTI - Living on the edge: Adaptive Optics+Lucky Imaging\nAU - Velasco, Sergio\nAD - AA(Instituto de Astrof\xedsica de Canarias)\nJO - IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\nY1 - 2016/03/1\nSP - 872\nUR - https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nN2 - Not Available

\nER -\n\n\nTY - Book Chapter\nTI - The Diversity of Nuclear Magnetic Resonance Spectroscopy\nAU - Liu, Corey W.\nAU - Alekseyev, Viktor Y.\nAU - Allwardt, Jeffrey R.\nAU - Bankovich, Alexander J.\nAU - Cade-Menun, Barbara J.\nAU - Davis, Ronald W.\nAU - Du, Lin-Shu\nAU - Garcia, K. Christopher\nAU - Herschlag, Daniel\nAU - Khosla, Chaitan\nAU - Kraut, Daniel A.\nAU - Li, Qing\nAU - Null, Brian\nAU - Puglisi, Joseph D.\nAU - Sigala, Paul A.\nAU - Stebbins, Jonathan F.\nAU - Varani, Luca\nAD - AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nJO - Biophysics and the Challenges of Emerging Threats\nY1 - 2009/01/1\nSP - 65\nKW - Physics\nUR - https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nN2 - The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\nDO - 10.1007/978-90-481-2368-1_5\nER -\n\n\nTY - Conference\nTI - Time Domain Exploration with the Palomar-QUEST Sky Survey\nAU - Mahabal, Ashish A.\nAU - Drake, A. J.\nAU - Djorgovski, S. G.\nAU - Donalek, C.\nAU - Glikman, E.\nAU - Graham, M. J.\nAU - Williams, R.\nAU - Baltay, C.\nAU - Rabinowitz, D.\nAU - PQ Team Caltech\nAU - Yale\nAU - NCSA\nAU - Indiana\nAU - , . . .\nAD - AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nJO - American Astronomical Society Meeting Abstracts #210\nVL - 210\nY1 - 2007/05/1\nSP - 21.04\nUR - https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nN2 - Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\nER -\n\n\nTY - Journal\nTI - Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nAU - ., S. N. Agbo\nAU - ., E. C. Okoroigwe\nJO - Research Journal of Physics\nVL - 1\nY1 - 2007/01/1\nSP - 35\nEP - 41\nUR - https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nN2 - Not Available

\nDO - 10.3923/rjp.2007.35.41\nSN - 1819-3463\nER -\n\n\nTY - Conference\nTI - Spacecraft navigation requirements\nAU - Miller, Judy L.\nAD - AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nJO - In AGARD\nY1 - 1995/06/1\nSP - 390\nEP - 405\nKW - Earth Orbits/ Navigation Aids/ Navigators/ Onboard Equipment/\nSpace Navigation/ Spacecraft Trajectories/ Support Systems/ Technology\nAssessment/ Technology Utilization/ Ascent Trajectories/ Reentry\nTrajectories/ Spacecraft/ Spacecraft Performance/ Spacecraft\nSurvivability/ Tradeoffs/ Weight (Mass)/ Space Communications,\nSpacecraft Communications, Command and Tracking\nUR - https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nN2 - Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\nER -\n\n\nTY - Book, Whole\nTI - Applied nonlinear dynamics: analytical, computational and experimental methods\nAU - Nayfeh, Ali H.\nAU - Balachandran, Balakumar\nJO - Wiley series in nonlinear science\nY1 - 1995/01/1\nUR - https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nN2 - Not Available

\nER -\n\n\nTY - Preprint\nTI - Applied Conformal Field Theory\nAU - Ginsparg, Paul\nJO - arXiv e-prints\nY1 - 1988/11/1\nSP - hep-th/9108028\nKW - High Energy Physics - Theory\nUR - https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nN2 - These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\nC1 - eprint: arXiv:hep-th/9108028\nER -\n\n\nTY - Journal\nTI - Autonomous navigation using lunar beacons\nAU - Khatib, A. R.\nAU - Ellis, J.\nAU - French, J.\nAU - Null, G.\nAU - Yunck, T.\nAU - Wu, S.\nAD - AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nJO - AIAA, Aerospace Sciences Meeting\nY1 - 1983/01/1\nKW - Artificial Satellites/ Autonomous Navigation/ Earth-Moon System/\nLunar Communication/ Radio Beacons/ Radio Navigation/ Space Navigation/\nDoppler Navigation/ Least Squares Method/ Orbit Calculation/ Space\nCommunications, Spacecraft Communications, Command and Tracking\nUR - https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nN2 - The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\nER -\n\n\nTY - Miscellaneous\nTI - Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nAU - Thornton, P. E.\nAU - Thornton, M. M.\nAU - Mayer, B. W.\nAU - Wilhelmi, N.\nAU - Wei, Y.\nAU - Devarakonda, R.\nAU - Cook, R.\nJO - Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\nY1 - 2012/04/1\nKW - Daymet\nUR - https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nN2 - Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\nDO - 10.3334/ORNLDAAC/1219\nER -\n\n\nTY - Journal\nTI - Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nAU - Dhaygude, Akanksha\nAU - Desai, Shantanu\nAD - AA(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India), AB(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India ;)\nJO - European Physical Journal C\nY1 - 2020/02/1\nKW - Astrophysics - High Energy Astrophysical Phenomena/ Astrophysics -\nInstrumentation and Methods for Astrophysics/ Nuclear Experiment\nUR - https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\nN2 - Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\nDO - 10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\nC1 - eprint: arXiv:1912.06970\nER -\n\n\n'} -data_refman= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': u'TY - JOUR\nTI - Book reviews\nJO - Weather\nVL - 73\nY1 - 2018/01/1\nSP - 35\nEP - 35\nUR - https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nN2 - Not Available

\nDO - 10.1002/wea.3072\nSN - 0043-1656\nER -\n\n\nTY - JOUR\nTI - 2D Materials: maintaining editorial quality\nAU - Fal\'ko, Vladimir\nAU - Thomas, Ceri-Wyn\nAD - AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\nJO - 2D Materials\nVL - 5\nY1 - 2018/01/1\nSP - 010201\nUR - https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nN2 - Not Available

\nDO - 10.1088/2053-1583/aa9403\nSN - 2053-1583\nER -\n\n\nTY - JOUR\nTI - Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nAU - Parkin, Stuart\nAU - Chantrell, Roy\nAU - Chang, Ching-Ray\nJO - Spin\nVL - 8\nY1 - 2018/01/1\nSP - 1877001\nUR - https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nN2 - Not Available

\nDO - 10.1142/S2010324718770015\nER -\n\n\nTY - JOUR\nTI - Millimeter Astronomy\nAU - Dessauges-Zavadsky, Miroslava\nAU - Pfenniger, Daniel\nJO - Saas-Fee Advanced Course\nVL - 38\nY1 - 2018/01/1\nKW - Physics\nUR - https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nN2 - Not Available

\nDO - 10.1007/978-3-662-57546-8\nER -\n\n\nTY - JOUR\nTI - Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nAU - Pustilnik, M.\nAU - van Heck, B.\nAU - Lutchyn, R. M.\nAU - Glazman, L. I.\nJO - Physical Review Letters\nVL - 120\nY1 - 2018/01/1\nSP - 029901\nUR - https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nN2 - Not Available

\nDO - 10.1103/PhysRevLett.120.029901\nSN - 0031-9007\nER -\n\n\nTY - Thesis/Dissertation\nTI - Resolving Gas-Phase Metallicity In Galaxies\nAU - Carton, David\nAD - AA(Leiden University)\nJO - Ph.D. Thesis\nY1 - 2017/06/1\nKW - galaxies: evolution\nKW - galaxies: abundances\nKW - galaxies: ISM\nUR - https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nN2 - Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\nDO - 10.5281/zenodo.581221\nER -\n\n\nTY - JOUR\nTI - A 3D View of a Supernova Remnant\nAU - Kohler, Susanna\nJO - AAS Nova Highlights\nY1 - 2017/06/1\nSP - 2388\nKW - Features\nKW - Highlights\nKW - interstellar medium\nKW - stellar evolution\nKW - supernova remnant\nKW - supernovae\nKW - white dwarfs\nUR - https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nN2 - The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\nER -\n\n\nTY - JOUR\nTI - Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nAU - Green, D. W. E.\nJO - Central Bureau Electronic Telegrams\nVL - 4403\nY1 - 2017/06/1\nSP - 2\nUR - https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nN2 - A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\nER -\n\n\nTY - MISC\nTI - sick: Spectroscopic inference crank\nAU - Casey, Andrew R.\nJO - Astrophysics Source Code Library\nY1 - 2017/06/1\nSP - ascl:1706.009\nKW - Software\nUR - https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nN2 - sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\nC1 - eprint: ascl:1706.009\nER -\n\n\nTY - JOUR\nTI - VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nAU - Siltala, J.\nAU - Jetsu, L.\nAU - Hackman, T.\nAU - Henry, G. W.\nAU - Immonen, L.\nAU - Kajatkari, P.\nAU - Lankinen, J.\nAU - Lehtinen, J.\nAU - Monira, S.\nAU - Nikbakhsh, S.\nAU - Viitanen, A.\nAU - Viuho, J.\nAU - Willamo, T.\nJO - VizieR Online Data Catalog\nY1 - 2017/05/1\nSP - J/AN/338/453\nKW - Stars: variable\nUR - https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nN2 - The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\nER -\n\n\nTY - JOUR\nTI - V694 Mon (MWC 560) spectroscopy requested\nAU - Waagen, Elizabeth O.\nAD - AA(AAVSO)\nJO - AAVSO Special Notice\nVL - 429\nY1 - 2017/05/1\nSP - 1\nKW - astronomical databases: miscellaneous\nKW - binaries: symbiotic\nKW - stars: individual (V694 Mon\nKW - MWC 560)\nUR - https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nN2 - The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi P\xe9ter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\nER -\n\n\nTY - MISC\nTI - Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nAU - Yan, Lin\nJO - Spitzer Proposal\nY1 - 2017/04/1\nSP - 13168\nUR - https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nN2 - ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\nER -\n\n\nTY - Thesis/Dissertation\nTI - Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAU - Azankpo, Severin\nAD - AA(University of Stellenbosch)\nJO - Masters Thesis\nY1 - 2017/03/1\nSP - 2\nUR - https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nN2 - The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\nER -\n\n\nTY - RPRT\nTI - The penumbral Moon\'s eclipse form 16 september 2016\nAU - Rotaru, Adrian\nAU - Pteancu, Mircea\nAU - Zaharia, Cristian\nAD - AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nJO - http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\nY1 - 2016/10/1\nKW - THE MOON\nKW - ECLIPSES\nKW - PARTIAL\nKW - PENUMBRAL\nKW - ASTROPHOTOGRAPHY\nUR - https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nN2 - The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\nER -\n\n\nTY - CONF\nTI - Living on the edge: Adaptive Optics+Lucky Imaging\nAU - Velasco, Sergio\nAD - AA(Instituto de Astrof\xedsica de Canarias)\nJO - IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\nY1 - 2016/03/1\nSP - 872\nUR - https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nN2 - Not Available

\nER -\n\n\nTY - CHAP\nTI - The Diversity of Nuclear Magnetic Resonance Spectroscopy\nAU - Liu, Corey W.\nAU - Alekseyev, Viktor Y.\nAU - Allwardt, Jeffrey R.\nAU - Bankovich, Alexander J.\nAU - Cade-Menun, Barbara J.\nAU - Davis, Ronald W.\nAU - Du, Lin-Shu\nAU - Garcia, K. Christopher\nAU - Herschlag, Daniel\nAU - Khosla, Chaitan\nAU - Kraut, Daniel A.\nAU - Li, Qing\nAU - Null, Brian\nAU - Puglisi, Joseph D.\nAU - Sigala, Paul A.\nAU - Stebbins, Jonathan F.\nAU - Varani, Luca\nAD - AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nJO - Biophysics and the Challenges of Emerging Threats\nY1 - 2009/01/1\nSP - 65\nKW - Physics\nUR - https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nN2 - The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\nDO - 10.1007/978-90-481-2368-1_5\nER -\n\n\nTY - CONF\nTI - Time Domain Exploration with the Palomar-QUEST Sky Survey\nAU - Mahabal, Ashish A.\nAU - Drake, A. J.\nAU - Djorgovski, S. G.\nAU - Donalek, C.\nAU - Glikman, E.\nAU - Graham, M. J.\nAU - Williams, R.\nAU - Baltay, C.\nAU - Rabinowitz, D.\nAU - PQ Team Caltech\nAU - Yale\nAU - NCSA\nAU - Indiana\nAU - , . . .\nAD - AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nJO - American Astronomical Society Meeting Abstracts #210\nVL - 210\nY1 - 2007/05/1\nSP - 21.04\nUR - https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nN2 - Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\nER -\n\n\nTY - JOUR\nTI - Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nAU - ., S. N. Agbo\nAU - ., E. C. Okoroigwe\nJO - Research Journal of Physics\nVL - 1\nY1 - 2007/01/1\nSP - 35\nEP - 41\nUR - https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nN2 - Not Available

\nDO - 10.3923/rjp.2007.35.41\nSN - 1819-3463\nER -\n\n\nTY - CONF\nTI - Spacecraft navigation requirements\nAU - Miller, Judy L.\nAD - AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nJO - In AGARD\nY1 - 1995/06/1\nSP - 390\nEP - 405\nKW - Earth Orbits\nKW - Navigation Aids\nKW - Navigators\nKW - Onboard Equipment\nKW - Space Navigation\nKW - Spacecraft Trajectories\nKW - Support Systems\nKW - Technology Assessment\nKW - Technology Utilization\nKW - Ascent Trajectories\nKW - Reentry Trajectories\nKW - Spacecraft\nKW - Spacecraft Performance\nKW - Spacecraft Survivability\nKW - Tradeoffs\nKW - Weight (Mass)\nKW - Space Communications, Spacecraft Communications, Command and Tracking\nUR - https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nN2 - Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\nER -\n\n\nTY - BOOK\nTI - Applied nonlinear dynamics: analytical, computational and experimental methods\nAU - Nayfeh, Ali H.\nAU - Balachandran, Balakumar\nJO - Wiley series in nonlinear science\nY1 - 1995/01/1\nUR - https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nN2 - Not Available

\nER -\n\n\nTY - Preprint\nTI - Applied Conformal Field Theory\nAU - Ginsparg, Paul\nJO - arXiv e-prints\nY1 - 1988/11/1\nSP - hep-th/9108028\nKW - High Energy Physics - Theory\nUR - https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nN2 - These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\nC1 - eprint: arXiv:hep-th/9108028\nER -\n\n\nTY - JOUR\nTI - Autonomous navigation using lunar beacons\nAU - Khatib, A. R.\nAU - Ellis, J.\nAU - French, J.\nAU - Null, G.\nAU - Yunck, T.\nAU - Wu, S.\nAD - AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nJO - AIAA, Aerospace Sciences Meeting\nY1 - 1983/01/1\nKW - Artificial Satellites\nKW - Autonomous Navigation\nKW - Earth-Moon System\nKW - Lunar Communication\nKW - Radio Beacons\nKW - Radio Navigation\nKW - Space Navigation\nKW - Doppler Navigation\nKW - Least Squares Method\nKW - Orbit Calculation\nKW - Space Communications, Spacecraft Communications, Command and Tracking\nUR - https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nN2 - The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\nER -\n\n\nTY - MISC\nTI - Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nAU - Thornton, P. E.\nAU - Thornton, M. M.\nAU - Mayer, B. W.\nAU - Wilhelmi, N.\nAU - Wei, Y.\nAU - Devarakonda, R.\nAU - Cook, R.\nJO - Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\nY1 - 2012/04/1\nKW - Daymet\nUR - https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nN2 - Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\nDO - 10.3334/ORNLDAAC/1219\nER -\n\n\n'} +data_refman= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': u'TY - JOUR\nTI - Book reviews\nJO - Weather\nVL - 73\nY1 - 2018/01/1\nSP - 35\nEP - 35\nUR - https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nN2 - Not Available

\nDO - 10.1002/wea.3072\nSN - 0043-1656\nER -\n\n\nTY - JOUR\nTI - 2D Materials: maintaining editorial quality\nAU - Fal\'ko, Vladimir\nAU - Thomas, Ceri-Wyn\nAD - AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\nJO - 2D Materials\nVL - 5\nY1 - 2018/01/1\nSP - 010201\nUR - https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nN2 - Not Available

\nDO - 10.1088/2053-1583/aa9403\nSN - 2053-1583\nER -\n\n\nTY - JOUR\nTI - Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nAU - Parkin, Stuart\nAU - Chantrell, Roy\nAU - Chang, Ching-Ray\nJO - Spin\nVL - 8\nY1 - 2018/01/1\nSP - 1877001\nUR - https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nN2 - Not Available

\nDO - 10.1142/S2010324718770015\nER -\n\n\nTY - JOUR\nTI - Millimeter Astronomy\nAU - Dessauges-Zavadsky, Miroslava\nAU - Pfenniger, Daniel\nJO - Saas-Fee Advanced Course\nVL - 38\nY1 - 2018/01/1\nKW - Physics\nUR - https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nN2 - Not Available

\nDO - 10.1007/978-3-662-57546-8\nER -\n\n\nTY - JOUR\nTI - Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nAU - Pustilnik, M.\nAU - van Heck, B.\nAU - Lutchyn, R. M.\nAU - Glazman, L. I.\nJO - Physical Review Letters\nVL - 120\nY1 - 2018/01/1\nSP - 029901\nUR - https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nN2 - Not Available

\nDO - 10.1103/PhysRevLett.120.029901\nSN - 0031-9007\nER -\n\n\nTY - Thesis/Dissertation\nTI - Resolving Gas-Phase Metallicity In Galaxies\nAU - Carton, David\nAD - AA(Leiden University)\nJO - Ph.D. Thesis\nY1 - 2017/06/1\nKW - galaxies: evolution\nKW - galaxies: abundances\nKW - galaxies: ISM\nUR - https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nN2 - Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\nDO - 10.5281/zenodo.581221\nER -\n\n\nTY - JOUR\nTI - A 3D View of a Supernova Remnant\nAU - Kohler, Susanna\nJO - AAS Nova Highlights\nY1 - 2017/06/1\nSP - 2388\nKW - Features\nKW - Highlights\nKW - interstellar medium\nKW - stellar evolution\nKW - supernova remnant\nKW - supernovae\nKW - white dwarfs\nUR - https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nN2 - The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\nER -\n\n\nTY - JOUR\nTI - Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nAU - Green, D. W. E.\nJO - Central Bureau Electronic Telegrams\nVL - 4403\nY1 - 2017/06/1\nSP - 2\nUR - https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nN2 - A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\nER -\n\n\nTY - MISC\nTI - sick: Spectroscopic inference crank\nAU - Casey, Andrew R.\nJO - Astrophysics Source Code Library\nY1 - 2017/06/1\nSP - ascl:1706.009\nKW - Software\nUR - https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nN2 - sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\nC1 - eprint: ascl:1706.009\nER -\n\n\nTY - JOUR\nTI - VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nAU - Siltala, J.\nAU - Jetsu, L.\nAU - Hackman, T.\nAU - Henry, G. W.\nAU - Immonen, L.\nAU - Kajatkari, P.\nAU - Lankinen, J.\nAU - Lehtinen, J.\nAU - Monira, S.\nAU - Nikbakhsh, S.\nAU - Viitanen, A.\nAU - Viuho, J.\nAU - Willamo, T.\nJO - VizieR Online Data Catalog\nY1 - 2017/05/1\nSP - J/AN/338/453\nKW - Stars: variable\nUR - https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nN2 - The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\nER -\n\n\nTY - JOUR\nTI - V694 Mon (MWC 560) spectroscopy requested\nAU - Waagen, Elizabeth O.\nAD - AA(AAVSO)\nJO - AAVSO Special Notice\nVL - 429\nY1 - 2017/05/1\nSP - 1\nKW - astronomical databases: miscellaneous\nKW - binaries: symbiotic\nKW - stars: individual (V694 Mon\nKW - MWC 560)\nUR - https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nN2 - The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi P\xe9ter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\nER -\n\n\nTY - MISC\nTI - Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nAU - Yan, Lin\nJO - Spitzer Proposal\nY1 - 2017/04/1\nSP - 13168\nUR - https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nN2 - ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\nER -\n\n\nTY - Thesis/Dissertation\nTI - Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAU - Azankpo, Severin\nAD - AA(University of Stellenbosch)\nJO - Masters Thesis\nY1 - 2017/03/1\nSP - 2\nUR - https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nN2 - The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\nER -\n\n\nTY - RPRT\nTI - The penumbral Moon\'s eclipse form 16 september 2016\nAU - Rotaru, Adrian\nAU - Pteancu, Mircea\nAU - Zaharia, Cristian\nAD - AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nJO - http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\nY1 - 2016/10/1\nKW - THE MOON\nKW - ECLIPSES\nKW - PARTIAL\nKW - PENUMBRAL\nKW - ASTROPHOTOGRAPHY\nUR - https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nN2 - The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\nER -\n\n\nTY - CONF\nTI - Living on the edge: Adaptive Optics+Lucky Imaging\nAU - Velasco, Sergio\nAD - AA(Instituto de Astrof\xedsica de Canarias)\nJO - IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\nY1 - 2016/03/1\nSP - 872\nUR - https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nN2 - Not Available

\nER -\n\n\nTY - CHAP\nTI - The Diversity of Nuclear Magnetic Resonance Spectroscopy\nAU - Liu, Corey W.\nAU - Alekseyev, Viktor Y.\nAU - Allwardt, Jeffrey R.\nAU - Bankovich, Alexander J.\nAU - Cade-Menun, Barbara J.\nAU - Davis, Ronald W.\nAU - Du, Lin-Shu\nAU - Garcia, K. Christopher\nAU - Herschlag, Daniel\nAU - Khosla, Chaitan\nAU - Kraut, Daniel A.\nAU - Li, Qing\nAU - Null, Brian\nAU - Puglisi, Joseph D.\nAU - Sigala, Paul A.\nAU - Stebbins, Jonathan F.\nAU - Varani, Luca\nAD - AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nJO - Biophysics and the Challenges of Emerging Threats\nY1 - 2009/01/1\nSP - 65\nKW - Physics\nUR - https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nN2 - The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\nDO - 10.1007/978-90-481-2368-1_5\nER -\n\n\nTY - CONF\nTI - Time Domain Exploration with the Palomar-QUEST Sky Survey\nAU - Mahabal, Ashish A.\nAU - Drake, A. J.\nAU - Djorgovski, S. G.\nAU - Donalek, C.\nAU - Glikman, E.\nAU - Graham, M. J.\nAU - Williams, R.\nAU - Baltay, C.\nAU - Rabinowitz, D.\nAU - PQ Team Caltech\nAU - Yale\nAU - NCSA\nAU - Indiana\nAU - , . . .\nAD - AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nJO - American Astronomical Society Meeting Abstracts #210\nVL - 210\nY1 - 2007/05/1\nSP - 21.04\nUR - https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nN2 - Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\nER -\n\n\nTY - JOUR\nTI - Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nAU - ., S. N. Agbo\nAU - ., E. C. Okoroigwe\nJO - Research Journal of Physics\nVL - 1\nY1 - 2007/01/1\nSP - 35\nEP - 41\nUR - https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nN2 - Not Available

\nDO - 10.3923/rjp.2007.35.41\nSN - 1819-3463\nER -\n\n\nTY - CONF\nTI - Spacecraft navigation requirements\nAU - Miller, Judy L.\nAD - AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nJO - In AGARD\nY1 - 1995/06/1\nSP - 390\nEP - 405\nKW - Earth Orbits\nKW - Navigation Aids\nKW - Navigators\nKW - Onboard Equipment\nKW - Space Navigation\nKW - Spacecraft Trajectories\nKW - Support Systems\nKW - Technology Assessment\nKW - Technology Utilization\nKW - Ascent Trajectories\nKW - Reentry Trajectories\nKW - Spacecraft\nKW - Spacecraft Performance\nKW - Spacecraft Survivability\nKW - Tradeoffs\nKW - Weight (Mass)\nKW - Space Communications, Spacecraft Communications, Command and Tracking\nUR - https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nN2 - Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\nER -\n\n\nTY - BOOK\nTI - Applied nonlinear dynamics: analytical, computational and experimental methods\nAU - Nayfeh, Ali H.\nAU - Balachandran, Balakumar\nJO - Wiley series in nonlinear science\nY1 - 1995/01/1\nUR - https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nN2 - Not Available

\nER -\n\n\nTY - Preprint\nTI - Applied Conformal Field Theory\nAU - Ginsparg, Paul\nJO - arXiv e-prints\nY1 - 1988/11/1\nSP - hep-th/9108028\nKW - High Energy Physics - Theory\nUR - https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nN2 - These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\nC1 - eprint: arXiv:hep-th/9108028\nER -\n\n\nTY - JOUR\nTI - Autonomous navigation using lunar beacons\nAU - Khatib, A. R.\nAU - Ellis, J.\nAU - French, J.\nAU - Null, G.\nAU - Yunck, T.\nAU - Wu, S.\nAD - AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nJO - AIAA, Aerospace Sciences Meeting\nY1 - 1983/01/1\nKW - Artificial Satellites\nKW - Autonomous Navigation\nKW - Earth-Moon System\nKW - Lunar Communication\nKW - Radio Beacons\nKW - Radio Navigation\nKW - Space Navigation\nKW - Doppler Navigation\nKW - Least Squares Method\nKW - Orbit Calculation\nKW - Space Communications, Spacecraft Communications, Command and Tracking\nUR - https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nN2 - The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\nER -\n\n\nTY - MISC\nTI - Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nAU - Thornton, P. E.\nAU - Thornton, M. M.\nAU - Mayer, B. W.\nAU - Wilhelmi, N.\nAU - Wei, Y.\nAU - Devarakonda, R.\nAU - Cook, R.\nJO - Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\nY1 - 2012/04/1\nKW - Daymet\nUR - https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nN2 - Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\nDO - 10.3334/ORNLDAAC/1219\nER -\n\n\nTY - JOUR\nTI - Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nAU - Dhaygude, Akanksha\nAU - Desai, Shantanu\nAD - AA(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India), AB(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India ;)\nJO - European Physical Journal C\nY1 - 2020/02/1\nKW - Astrophysics - High Energy Astrophysical Phenomena\nKW - Astrophysics - Instrumentation and Methods for Astrophysics\nKW - Nuclear Experiment\nUR - https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\nN2 - Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\nDO - 10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\nC1 - eprint: arXiv:1912.06970\nER -\n\n\n'} -data_refworks= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': 'RT Journal\nT1 Book reviews\nJF Weather\nVO 73\nYR 2018\nFD 2018/01/1\nSP 35\nOP 35\nLK https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nAB Not Available

\nDO DOI: 10.1002/wea.3072\nSN 0043-1656\n\n\nRT Journal\nT1 2D Materials: maintaining editorial quality\nA1 Fal\'ko, Vladimir\nA1 Thomas, Ceri-Wyn\nAD AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\nJF 2D Materials\nVO 5\nYR 2018\nFD 2018/01/1\nSP 010201\nLK https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nAB Not Available

\nDO DOI: 10.1088/2053-1583/aa9403\nSN 2053-1583\n\n\nRT Journal\nT1 Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nA1 Parkin, Stuart\nA1 Chantrell, Roy\nA1 Chang, Ching-Ray\nJF Spin\nVO 8\nYR 2018\nFD 2018/01/1\nSP 1877001\nLK https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nAB Not Available

\nDO DOI: 10.1142/S2010324718770015\n\n\nRT Journal\nT1 Millimeter Astronomy\nA1 Dessauges-Zavadsky, Miroslava\nA1 Pfenniger, Daniel\nJF Saas-Fee Advanced Course\nVO 38\nYR 2018\nFD 2018/01/1\nK1 Physics\nLK https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nAB Not Available

\nDO DOI: 10.1007/978-3-662-57546-8\n\n\nRT Journal\nT1 Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nA1 Pustilnik, M.\nA1 van Heck, B.\nA1 Lutchyn, R. M.\nA1 Glazman, L. I.\nJF Physical Review Letters\nVO 120\nYR 2018\nFD 2018/01/1\nSP 029901\nLK https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nAB Not Available

\nDO DOI: 10.1103/PhysRevLett.120.029901\nSN 0031-9007\n\n\nRT Thesis/Dissertation\nT1 Resolving Gas-Phase Metallicity In Galaxies\nA1 Carton, David\nAD AA(Leiden University)\nJF Ph.D. Thesis\nYR 2017\nFD 2017/06/1\nK1 galaxies: evolution\nK1 galaxies: abundances\nK1 galaxies: ISM\nLK https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nAB Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\nDO DOI: 10.5281/zenodo.581221\n\n\nRT Journal\nT1 A 3D View of a Supernova Remnant\nA1 Kohler, Susanna\nJF AAS Nova Highlights\nYR 2017\nFD 2017/06/1\nSP 2388\nK1 Features\nK1 Highlights\nK1 interstellar medium\nK1 stellar evolution\nK1 supernova remnant\nK1 supernovae\nK1 white dwarfs\nLK https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nAB The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\n\n\nRT Journal\nT1 Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nA1 Green, D. W. E.\nJF Central Bureau Electronic Telegrams\nVO 4403\nYR 2017\nFD 2017/06/1\nSP 2\nLK https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nAB A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\n\n\nRT Generic\nT1 sick: Spectroscopic inference crank\nA1 Casey, Andrew R.\nJF Astrophysics Source Code Library\nYR 2017\nFD 2017/06/1\nSP ascl:1706.009\nK1 Software\nLK https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nAB sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\nDO eprintid: ascl:1706.009\n\n\nRT Journal\nT1 VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nA1 Siltala, J.\nA1 Jetsu, L.\nA1 Hackman, T.\nA1 Henry, G. W.\nA1 Immonen, L.\nA1 Kajatkari, P.\nA1 Lankinen, J.\nA1 Lehtinen, J.\nA1 Monira, S.\nA1 Nikbakhsh, S.\nA1 Viitanen, A.\nA1 Viuho, J.\nA1 Willamo, T.\nJF VizieR Online Data Catalog\nYR 2017\nFD 2017/05/1\nSP J/AN/338/453\nK1 Stars: variable\nLK https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nNO phot.dat 2930x19 Differential photometry of BM CVn; phot_mlc.dat 2930x19\nDifferential photometry of BM CVn with MLC removed; res.dat 1319x185\n*Numerical results of the CPS analysis; res_mlc.dat 1319x185 *Results of\nthe CPS analysis with MLC removed\nAB The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\n\n\nRT Journal\nT1 V694 Mon (MWC 560) spectroscopy requested\nA1 Waagen, Elizabeth O.\nAD AA(AAVSO)\nJF AAVSO Special Notice\nVO 429\nYR 2017\nFD 2017/05/1\nSP 1\nK1 astronomical databases: miscellaneous\nK1 binaries: symbiotic\nK1 stars: individual (V694 Mon\nK1 MWC 560)\nLK https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nAB The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\n\n\nRT Generic\nT1 Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nA1 Yan, Lin\nJF Spitzer Proposal\nYR 2017\nFD 2017/04/1\nSP 13168\nLK https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nAB ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\n\n\nRT Thesis/Dissertation\nT1 Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nA1 Azankpo, Severin\nAD AA(University of Stellenbosch)\nJF Masters Thesis\nYR 2017\nFD 2017/03/1\nSP 2\nLK https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nAB The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\n\n\nRT Report\nT1 The penumbral Moon\'s eclipse form 16 september 2016\nA1 Rotaru, Adrian\nA1 Pteancu, Mircea\nA1 Zaharia, Cristian\nAD AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nJF http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\nYR 2016\nFD 2016/10/1\nK1 THE MOON\nK1 ECLIPSES\nK1 PARTIAL\nK1 PENUMBRAL\nK1 ASTROPHOTOGRAPHY\nLK https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nAB The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\n\n\nRT Conference Proceeding\nT1 Living on the edge: Adaptive Optics+Lucky Imaging\nA1 Velasco, Sergio\nAD AA(Instituto de Astrofísica de Canarias)\nJF IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\nYR 2016\nFD 2016/03/1\nSP 872\nLK https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nAB Not Available

\n\n\nRT Book, Chapter\nT1 The Diversity of Nuclear Magnetic Resonance Spectroscopy\nA1 Liu, Corey W.\nA1 Alekseyev, Viktor Y.\nA1 Allwardt, Jeffrey R.\nA1 Bankovich, Alexander J.\nA1 Cade-Menun, Barbara J.\nA1 Davis, Ronald W.\nA1 Du, Lin-Shu\nA1 Garcia, K. Christopher\nA1 Herschlag, Daniel\nA1 Khosla, Chaitan\nA1 Kraut, Daniel A.\nA1 Li, Qing\nA1 Null, Brian\nA1 Puglisi, Joseph D.\nA1 Sigala, Paul A.\nA1 Stebbins, Jonathan F.\nA1 Varani, Luca\nA2 Puglisi, Joseph D.\nAD AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nJF Biophysics and the Challenges of Emerging Threats\nYR 2009\nFD 2009/01/1\nSP 65\nK1 Physics\nLK https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nAB The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\nDO DOI: 10.1007/978-90-481-2368-1_5\n\n\nRT Conference Proceeding\nT1 Time Domain Exploration with the Palomar-QUEST Sky Survey\nA1 Mahabal, Ashish A.\nA1 Drake, A. J.\nA1 Djorgovski, S. G.\nA1 Donalek, C.\nA1 Glikman, E.\nA1 Graham, M. J.\nA1 Williams, R.\nA1 Baltay, C.\nA1 Rabinowitz, D.\nA1 PQ Team Caltech\nA1 Yale\nA1 NCSA\nA1 Indiana\nA1 , . . .\nAD AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nJF American Astronomical Society Meeting Abstracts #210\nVO 210\nYR 2007\nFD 2007/05/1\nSP 21.04\nLK https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nAB Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\n\n\nRT Journal\nT1 Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nA1 ., S. N. Agbo\nA1 ., E. C. Okoroigwe\nJF Research Journal of Physics\nVO 1\nYR 2007\nFD 2007/01/1\nSP 35\nOP 41\nLK https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nAB Not Available

\nDO DOI: 10.3923/rjp.2007.35.41\nSN 1819-3463\n\n\nRT Conference Proceeding\nT1 Spacecraft navigation requirements\nA1 Miller, Judy L.\nAD AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nJF In AGARD\nYR 1995\nFD 1995/06/1\nSP 390\nOP 405\nK1 Earth Orbits\nK1 Navigation Aids\nK1 Navigators\nK1 Onboard Equipment\nK1 Space Navigation\nK1 Spacecraft Trajectories\nK1 Support Systems\nK1 Technology Assessment\nK1 Technology Utilization\nK1 Ascent Trajectories\nK1 Reentry Trajectories\nK1 Spacecraft\nK1 Spacecraft Performance\nK1 Spacecraft Survivability\nK1 Tradeoffs\nK1 Weight (Mass)\nK1 Space Communications, Spacecraft Communications, Command and Tracking\nLK https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nAB Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\n\n\nRT Book, Whole\nT1 Applied nonlinear dynamics: analytical, computational and experimental methods\nA1 Nayfeh, Ali H.\nA1 Balachandran, Balakumar\nJF Wiley series in nonlinear science\nYR 1995\nFD 1995/01/1\nLK https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nAB Not Available

\n\n\nRT Preprint\nT1 Applied Conformal Field Theory\nA1 Ginsparg, Paul\nJF arXiv e-prints\nYR 1988\nFD 1988/11/1\nSP hep-th/9108028\nK1 High Energy Physics - Theory\nLK https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nAB These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\nDO eprintid: arXiv:hep-th/9108028\n\n\nRT Journal\nT1 Autonomous navigation using lunar beacons\nA1 Khatib, A. R.\nA1 Ellis, J.\nA1 French, J.\nA1 Null, G.\nA1 Yunck, T.\nA1 Wu, S.\nAD AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nJF AIAA, Aerospace Sciences Meeting\nYR 1983\nFD 1983/01/1\nK1 Artificial Satellites\nK1 Autonomous Navigation\nK1 Earth-Moon System\nK1 Lunar Communication\nK1 Radio Beacons\nK1 Radio Navigation\nK1 Space Navigation\nK1 Doppler Navigation\nK1 Least Squares Method\nK1 Orbit Calculation\nK1 Space Communications, Spacecraft Communications, Command and Tracking\nLK https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nAB The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\n\n\nRT Generic\nT1 Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nA1 Thornton, P. E.\nA1 Thornton, M. M.\nA1 Mayer, B. W.\nA1 Wilhelmi, N.\nA1 Wei, Y.\nA1 Devarakonda, R.\nA1 Cook, R.\nJF Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\nYR 2012\nFD 2012/04/1\nK1 Daymet\nLK https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nAB Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\nDO DOI: 10.3334/ORNLDAAC/1219\n\n\n'} +data_refworks= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': 'RT Journal\nT1 Book reviews\nJF Weather\nVO 73\nYR 2018\nFD 2018/01/1\nSP 35\nOP 35\nLK https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nAB Not Available

\nDO DOI: 10.1002/wea.3072\nSN 0043-1656\n\n\nRT Journal\nT1 2D Materials: maintaining editorial quality\nA1 Fal\'ko, Vladimir\nA1 Thomas, Ceri-Wyn\nAD AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\nJF 2D Materials\nVO 5\nYR 2018\nFD 2018/01/1\nSP 010201\nLK https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nAB Not Available

\nDO DOI: 10.1088/2053-1583/aa9403\nSN 2053-1583\n\n\nRT Journal\nT1 Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nA1 Parkin, Stuart\nA1 Chantrell, Roy\nA1 Chang, Ching-Ray\nJF Spin\nVO 8\nYR 2018\nFD 2018/01/1\nSP 1877001\nLK https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nAB Not Available

\nDO DOI: 10.1142/S2010324718770015\n\n\nRT Journal\nT1 Millimeter Astronomy\nA1 Dessauges-Zavadsky, Miroslava\nA1 Pfenniger, Daniel\nJF Saas-Fee Advanced Course\nVO 38\nYR 2018\nFD 2018/01/1\nK1 Physics\nLK https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nAB Not Available

\nDO DOI: 10.1007/978-3-662-57546-8\n\n\nRT Journal\nT1 Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nA1 Pustilnik, M.\nA1 van Heck, B.\nA1 Lutchyn, R. M.\nA1 Glazman, L. I.\nJF Physical Review Letters\nVO 120\nYR 2018\nFD 2018/01/1\nSP 029901\nLK https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nAB Not Available

\nDO DOI: 10.1103/PhysRevLett.120.029901\nSN 0031-9007\n\n\nRT Thesis/Dissertation\nT1 Resolving Gas-Phase Metallicity In Galaxies\nA1 Carton, David\nAD AA(Leiden University)\nJF Ph.D. Thesis\nYR 2017\nFD 2017/06/1\nK1 galaxies: evolution\nK1 galaxies: abundances\nK1 galaxies: ISM\nLK https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nAB Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\nDO DOI: 10.5281/zenodo.581221\n\n\nRT Journal\nT1 A 3D View of a Supernova Remnant\nA1 Kohler, Susanna\nJF AAS Nova Highlights\nYR 2017\nFD 2017/06/1\nSP 2388\nK1 Features\nK1 Highlights\nK1 interstellar medium\nK1 stellar evolution\nK1 supernova remnant\nK1 supernovae\nK1 white dwarfs\nLK https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nAB The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\n\n\nRT Journal\nT1 Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nA1 Green, D. W. E.\nJF Central Bureau Electronic Telegrams\nVO 4403\nYR 2017\nFD 2017/06/1\nSP 2\nLK https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nAB A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\n\n\nRT Generic\nT1 sick: Spectroscopic inference crank\nA1 Casey, Andrew R.\nJF Astrophysics Source Code Library\nYR 2017\nFD 2017/06/1\nSP ascl:1706.009\nK1 Software\nLK https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nAB sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\nDO eprintid: ascl:1706.009\n\n\nRT Journal\nT1 VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nA1 Siltala, J.\nA1 Jetsu, L.\nA1 Hackman, T.\nA1 Henry, G. W.\nA1 Immonen, L.\nA1 Kajatkari, P.\nA1 Lankinen, J.\nA1 Lehtinen, J.\nA1 Monira, S.\nA1 Nikbakhsh, S.\nA1 Viitanen, A.\nA1 Viuho, J.\nA1 Willamo, T.\nJF VizieR Online Data Catalog\nYR 2017\nFD 2017/05/1\nSP J/AN/338/453\nK1 Stars: variable\nLK https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nNO phot.dat 2930x19 Differential photometry of BM CVn; phot_mlc.dat 2930x19\nDifferential photometry of BM CVn with MLC removed; res.dat 1319x185\n*Numerical results of the CPS analysis; res_mlc.dat 1319x185 *Results of\nthe CPS analysis with MLC removed\nAB The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\n\n\nRT Journal\nT1 V694 Mon (MWC 560) spectroscopy requested\nA1 Waagen, Elizabeth O.\nAD AA(AAVSO)\nJF AAVSO Special Notice\nVO 429\nYR 2017\nFD 2017/05/1\nSP 1\nK1 astronomical databases: miscellaneous\nK1 binaries: symbiotic\nK1 stars: individual (V694 Mon\nK1 MWC 560)\nLK https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nAB The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\n\n\nRT Generic\nT1 Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nA1 Yan, Lin\nJF Spitzer Proposal\nYR 2017\nFD 2017/04/1\nSP 13168\nLK https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nAB ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\n\n\nRT Thesis/Dissertation\nT1 Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nA1 Azankpo, Severin\nAD AA(University of Stellenbosch)\nJF Masters Thesis\nYR 2017\nFD 2017/03/1\nSP 2\nLK https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nAB The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\n\n\nRT Report\nT1 The penumbral Moon\'s eclipse form 16 september 2016\nA1 Rotaru, Adrian\nA1 Pteancu, Mircea\nA1 Zaharia, Cristian\nAD AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nJF http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian\nYR 2016\nFD 2016/10/1\nK1 THE MOON\nK1 ECLIPSES\nK1 PARTIAL\nK1 PENUMBRAL\nK1 ASTROPHOTOGRAPHY\nLK https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nAB The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\n\n\nRT Conference Proceeding\nT1 Living on the edge: Adaptive Optics+Lucky Imaging\nA1 Velasco, Sergio\nAD AA(Instituto de Astrofísica de Canarias)\nJF IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias\nYR 2016\nFD 2016/03/1\nSP 872\nLK https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nAB Not Available

\n\n\nRT Book, Chapter\nT1 The Diversity of Nuclear Magnetic Resonance Spectroscopy\nA1 Liu, Corey W.\nA1 Alekseyev, Viktor Y.\nA1 Allwardt, Jeffrey R.\nA1 Bankovich, Alexander J.\nA1 Cade-Menun, Barbara J.\nA1 Davis, Ronald W.\nA1 Du, Lin-Shu\nA1 Garcia, K. Christopher\nA1 Herschlag, Daniel\nA1 Khosla, Chaitan\nA1 Kraut, Daniel A.\nA1 Li, Qing\nA1 Null, Brian\nA1 Puglisi, Joseph D.\nA1 Sigala, Paul A.\nA1 Stebbins, Jonathan F.\nA1 Varani, Luca\nA2 Puglisi, Joseph D.\nAD AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nJF Biophysics and the Challenges of Emerging Threats\nYR 2009\nFD 2009/01/1\nSP 65\nK1 Physics\nLK https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nAB The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\nDO DOI: 10.1007/978-90-481-2368-1_5\n\n\nRT Conference Proceeding\nT1 Time Domain Exploration with the Palomar-QUEST Sky Survey\nA1 Mahabal, Ashish A.\nA1 Drake, A. J.\nA1 Djorgovski, S. G.\nA1 Donalek, C.\nA1 Glikman, E.\nA1 Graham, M. J.\nA1 Williams, R.\nA1 Baltay, C.\nA1 Rabinowitz, D.\nA1 PQ Team Caltech\nA1 Yale\nA1 NCSA\nA1 Indiana\nA1 , . . .\nAD AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nJF American Astronomical Society Meeting Abstracts #210\nVO 210\nYR 2007\nFD 2007/05/1\nSP 21.04\nLK https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nAB Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\n\n\nRT Journal\nT1 Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nA1 ., S. N. Agbo\nA1 ., E. C. Okoroigwe\nJF Research Journal of Physics\nVO 1\nYR 2007\nFD 2007/01/1\nSP 35\nOP 41\nLK https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nAB Not Available

\nDO DOI: 10.3923/rjp.2007.35.41\nSN 1819-3463\n\n\nRT Conference Proceeding\nT1 Spacecraft navigation requirements\nA1 Miller, Judy L.\nAD AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nJF In AGARD\nYR 1995\nFD 1995/06/1\nSP 390\nOP 405\nK1 Earth Orbits\nK1 Navigation Aids\nK1 Navigators\nK1 Onboard Equipment\nK1 Space Navigation\nK1 Spacecraft Trajectories\nK1 Support Systems\nK1 Technology Assessment\nK1 Technology Utilization\nK1 Ascent Trajectories\nK1 Reentry Trajectories\nK1 Spacecraft\nK1 Spacecraft Performance\nK1 Spacecraft Survivability\nK1 Tradeoffs\nK1 Weight (Mass)\nK1 Space Communications, Spacecraft Communications, Command and Tracking\nLK https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nAB Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\n\n\nRT Book, Whole\nT1 Applied nonlinear dynamics: analytical, computational and experimental methods\nA1 Nayfeh, Ali H.\nA1 Balachandran, Balakumar\nJF Wiley series in nonlinear science\nYR 1995\nFD 1995/01/1\nLK https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nAB Not Available

\n\n\nRT Preprint\nT1 Applied Conformal Field Theory\nA1 Ginsparg, Paul\nJF arXiv e-prints\nYR 1988\nFD 1988/11/1\nSP hep-th/9108028\nK1 High Energy Physics - Theory\nLK https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nAB These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\nDO eprintid: arXiv:hep-th/9108028\n\n\nRT Journal\nT1 Autonomous navigation using lunar beacons\nA1 Khatib, A. R.\nA1 Ellis, J.\nA1 French, J.\nA1 Null, G.\nA1 Yunck, T.\nA1 Wu, S.\nAD AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nJF AIAA, Aerospace Sciences Meeting\nYR 1983\nFD 1983/01/1\nK1 Artificial Satellites\nK1 Autonomous Navigation\nK1 Earth-Moon System\nK1 Lunar Communication\nK1 Radio Beacons\nK1 Radio Navigation\nK1 Space Navigation\nK1 Doppler Navigation\nK1 Least Squares Method\nK1 Orbit Calculation\nK1 Space Communications, Spacecraft Communications, Command and Tracking\nLK https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nAB The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\n\n\nRT Generic\nT1 Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nA1 Thornton, P. E.\nA1 Thornton, M. M.\nA1 Mayer, B. W.\nA1 Wilhelmi, N.\nA1 Wei, Y.\nA1 Devarakonda, R.\nA1 Cook, R.\nJF Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC\nYR 2012\nFD 2012/04/1\nK1 Daymet\nLK https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nAB Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\nDO DOI: 10.3334/ORNLDAAC/1219\n\n\nRT Journal\nT1 Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nA1 Dhaygude, Akanksha\nA1 Desai, Shantanu\nAD AA(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India), AB(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India ;)\nJF European Physical Journal C\nYR 2020\nFD 2020/02/1\nK1 Astrophysics - High Energy Astrophysical Phenomena\nK1 Astrophysics - Instrumentation and Methods for Astrophysics\nK1 Nuclear Experiment\nLK https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\nAB Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\nDO DOI: 10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\nDO eprintid: arXiv:1912.06970\n\n\n'} -data_medlars= {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': 'PT - Journal Article\nTI - Book reviews\nTA - Wthr\nSO - Weather, vol. 73, issue 1, pp. 35-35\nVI - 73\nDP - 2018 Jan 01\nPG - 35-35\n4099- https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nAB - Not Available

\nIS - 0043-1656\n\n\nPT - Journal Article\nTI - 2D Materials: maintaining editorial quality\nAU - Fal\'ko, Vladimir\nAU - Thomas, Ceri-Wyn\nAD - AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\nTA - TDM\nSO - 2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\nVI - 5\nDP - 2018 Jan 01\nPG - 010201\n4099- https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nAB - Not Available

\nIS - 2053-1583\n\n\nPT - Journal Article\nTI - Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nAU - Parkin, Stuart\nAU - Chantrell, Roy\nAU - Chang, Ching-Ray\nTA - Spin\nSO - Spin, Volume 8, Issue 4, id. 1877001\nVI - 8\nDP - 2018 Jan 01\nPG - 1877001\n4099- https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nAB - Not Available

\n\n\nPT - Journal Article\nTI - Millimeter Astronomy\nAU - Dessauges-Zavadsky, Miroslava\nAU - Pfenniger, Daniel\nTA - SAAS\nSO - Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\nVI - 38\nDP - 2018 Jan 01\n4099- https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nAB - Not Available

\n\n\nPT - Journal Article\nTI - Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nAU - Pustilnik, M.\nAU - van Heck, B.\nAU - Lutchyn, R. M.\nAU - Glazman, L. I.\nTA - PhRvL\nSO - Physical Review Letters, Volume 120, Issue 2, id.029901\nVI - 120\nDP - 2018 Jan 01\nPG - 029901\n4099- https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nAB - Not Available

\nIS - 0031-9007\n\n\nPT - Thesis\nTI - Resolving Gas-Phase Metallicity In Galaxies\nAU - Carton, David\nAD - AA(Leiden University)\nTA - PhDT\nSO - PhD Thesis, Leiden University, 2017\nDP - 2017 Jun 01\n4099- https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nAB - Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\n\n\nPT - Journal Article\nTI - A 3D View of a Supernova Remnant\nAU - Kohler, Susanna\nTA - nova\nSO - AAS Nova Highlight, 14 Jun 2017, id.2388\nDP - 2017 Jun 01\nPG - 2388\n4099- https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nAB - The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\n\n\nPT - Journal Article\nTI - Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nAU - Green, D. W. E.\nTA - CBET\nSO - Central Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\nVI - 4403\nDP - 2017 Jun 01\nPG - 2\n4099- https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nAB - A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\n\n\nPT - Miscellaneous\nTI - sick: Spectroscopic inference crank\nAU - Casey, Andrew R.\nTA - ascl\nSO - Astrophysics Source Code Library, record ascl:1706.009\nDP - 2017 Jun 01\nPG - ascl:1706.009\n4099- https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nAB - sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\n\n\nPT - Journal Article\nTI - VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nAU - Siltala, J.\nAU - Jetsu, L.\nAU - Hackman, T.\nAU - Henry, G. W.\nAU - Immonen, L.\nAU - Kajatkari, P.\nAU - Lankinen, J.\nAU - Lehtinen, J.\nAU - Monira, S.\nAU - Nikbakhsh, S.\nAU - Viitanen, A.\nAU - Viuho, J.\nAU - Willamo, T.\nTA - yCat\nSO - VizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\nDP - 2017 May 01\nPG - J/AN/338/453\n4099- https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nAB - The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\n\n\nPT - Journal Article\nTI - V694 Mon (MWC 560) spectroscopy requested\nAU - Waagen, Elizabeth O.\nAD - AA(AAVSO)\nTA - AAVSN\nSO - AAVSO Special Notice #429\nVI - 429\nDP - 2017 May 01\nPG - 1\n4099- https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nAB - The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\n\n\nPT - Miscellaneous\nTI - Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nAU - Yan, Lin\nTA - sptz\nSO - Spitzer Proposal ID 13168\nDP - 2017 Apr 01\nPG - 13168\n4099- https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nAB - ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\n\n\nPT - Thesis\nTI - Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAU - Azankpo, Severin\nAD - AA(University of Stellenbosch)\nTA - MsT\nSO - Masters thesis, University of Stellenbosch, March 2017, 120 pages\nDP - 2017 Mar 01\nPG - 2\n4099- https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nAB - The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\n\n\nPT - Report\nTI - The penumbral Moon\'s eclipse form 16 september 2016\nAU - Rotaru, Adrian\nAU - Pteancu, Mircea\nAU - Zaharia, Cristian\nAD - AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nTA - emo6\nSO - http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\nDP - 2016 Oct 01\n4099- https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nAB - The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\n\n\nPT - Conference\nTI - Living on the edge: Adaptive Optics+Lucky Imaging\nAU - Velasco, Sergio\nAD - AA(Instituto de Astrofísica de Canarias)\nTA - iac\nSO - IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\nDP - 2016 Mar 01\nPG - 872\n4099- https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nAB - Not Available

\n\n\nPT - Book Chapter\nTI - The Diversity of Nuclear Magnetic Resonance Spectroscopy\nAU - Liu, Corey W.\nAU - Alekseyev, Viktor Y.\nAU - Allwardt, Jeffrey R.\nAU - Bankovich, Alexander J.\nAU - Cade-Menun, Barbara J.\nAU - Davis, Ronald W.\nAU - Du, Lin-Shu\nAU - Garcia, K. Christopher\nAU - Herschlag, Daniel\nAU - Khosla, Chaitan\nAU - Kraut, Daniel A.\nAU - Li, Qing\nAU - Null, Brian\nAU - Puglisi, Joseph D.\nAU - Sigala, Paul A.\nAU - Stebbins, Jonathan F.\nAU - Varani, Luca\nAD - AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nTA - bcet\nSO - Biophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\nDP - 2009 Jan 01\nPG - 65\n4099- https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nAB - The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\n\n\nPT - Conference\nTI - Time Domain Exploration with the Palomar-QUEST Sky Survey\nAU - Mahabal, Ashish A.\nAU - Drake, A. J.\nAU - Djorgovski, S. G.\nAU - Donalek, C.\nAU - Glikman, E.\nAU - Graham, M. J.\nAU - Williams, R.\nAU - Baltay, C.\nAU - Rabinowitz, D.\nAU - PQ Team Caltech\nAU - Yale\nAU - NCSA\nAU - Indiana\nAU - , . . .\nAD - AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nTA - AAS\nSO - American Astronomical Society Meeting 210, id.21.04\nVI - 210\nDP - 2007 May 01\nPG - 21.04\n4099- https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nAB - Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\n\n\nPT - Journal Article\nTI - Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nAU - ., S. N. Agbo\nAU - ., E. C. Okoroigwe\nTA - RJPh\nSO - Research Journal of Physics, vol. 1, issue 1, pp. 35-41\nVI - 1\nDP - 2007 Jan 01\nPG - 35-41\n4099- https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nAB - Not Available

\nIS - 1819-3463\n\n\nPT - Conference\nTI - Spacecraft navigation requirements\nAU - Miller, Judy L.\nAD - AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nTA - ans\nSO - In AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\nDP - 1995 Jun 01\nPG - 390-405\n4099- https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nAB - Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\n\n\nPT - Book\nTI - Applied nonlinear dynamics: analytical, computational and experimental methods\nAU - Nayfeh, Ali H.\nAU - Balachandran, Balakumar\nTA - anda\nSO - Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995\nDP - 1995 Jan 01\n4099- https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nAB - Not Available

\n\n\nPT - Preprint\nTI - Applied Conformal Field Theory\nAU - Ginsparg, Paul\nTA - arXiv\nSO - eprint arXiv:hep-th/9108028\nDP - 1988 Nov 01\nPG - hep-th/9108028\n4099- https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nAB - These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\n\n\nPT - Journal Article\nTI - Autonomous navigation using lunar beacons\nAU - Khatib, A. R.\nAU - Ellis, J.\nAU - French, J.\nAU - Null, G.\nAU - Yunck, T.\nAU - Wu, S.\nAD - AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nTA - aiaa\nSO - American Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\nDP - 1983 Jan 01\n4099- https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nAB - The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\n\n\nPT - Miscellaneous\nTI - Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nAU - Thornton, P. E.\nAU - Thornton, M. M.\nAU - Mayer, B. W.\nAU - Wilhelmi, N.\nAU - Wei, Y.\nAU - Devarakonda, R.\nAU - Cook, R.\nTA - ddsw\nSO - Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\nDP - 2012 Apr 01\n4099- https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nAB - Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\n\n\n'} +data_medlars= {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': 'PT - Journal Article\nTI - Book reviews\nTA - Wthr\nSO - Weather, vol. 73, issue 1, pp. 35-35\nVI - 73\nDP - 2018 Jan 01\nPG - 35-35\n4099- https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nAB - Not Available

\nIS - 0043-1656\n\n\nPT - Journal Article\nTI - 2D Materials: maintaining editorial quality\nAU - Fal\'ko, Vladimir\nAU - Thomas, Ceri-Wyn\nAD - AA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\nTA - TDM\nSO - 2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\nVI - 5\nDP - 2018 Jan 01\nPG - 010201\n4099- https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nAB - Not Available

\nIS - 2053-1583\n\n\nPT - Journal Article\nTI - Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nAU - Parkin, Stuart\nAU - Chantrell, Roy\nAU - Chang, Ching-Ray\nTA - Spin\nSO - Spin, Volume 8, Issue 4, id. 1877001\nVI - 8\nDP - 2018 Jan 01\nPG - 1877001\n4099- https://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nAB - Not Available

\n\n\nPT - Journal Article\nTI - Millimeter Astronomy\nAU - Dessauges-Zavadsky, Miroslava\nAU - Pfenniger, Daniel\nTA - SAAS\nSO - Millimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\nVI - 38\nDP - 2018 Jan 01\n4099- https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nAB - Not Available

\n\n\nPT - Journal Article\nTI - Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nAU - Pustilnik, M.\nAU - van Heck, B.\nAU - Lutchyn, R. M.\nAU - Glazman, L. I.\nTA - PhRvL\nSO - Physical Review Letters, Volume 120, Issue 2, id.029901\nVI - 120\nDP - 2018 Jan 01\nPG - 029901\n4099- https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nAB - Not Available

\nIS - 0031-9007\n\n\nPT - Thesis\nTI - Resolving Gas-Phase Metallicity In Galaxies\nAU - Carton, David\nAD - AA(Leiden University)\nTA - PhDT\nSO - PhD Thesis, Leiden University, 2017\nDP - 2017 Jun 01\n4099- https://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nAB - Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation.

Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies.

Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 < z < 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span>, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d < 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d > 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient.

Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 < z < 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas.

\n\n\nPT - Journal Article\nTI - A 3D View of a Supernova Remnant\nAU - Kohler, Susanna\nTA - nova\nSO - AAS Nova Highlight, 14 Jun 2017, id.2388\nDP - 2017 Jun 01\nPG - 2388\n4099- https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nAB - The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384

\n\n\nPT - Journal Article\nTI - Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nAU - Green, D. W. E.\nTA - CBET\nSO - Central Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\nVI - 4403\nDP - 2017 Jun 01\nPG - 2\n4099- https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nAB - A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).

\n\n\nPT - Miscellaneous\nTI - sick: Spectroscopic inference crank\nAU - Casey, Andrew R.\nTA - ascl\nSO - Astrophysics Source Code Library, record ascl:1706.009\nDP - 2017 Jun 01\nPG - ascl:1706.009\n4099- https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nAB - sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data.

\n\n\nPT - Journal Article\nTI - VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nAU - Siltala, J.\nAU - Jetsu, L.\nAU - Hackman, T.\nAU - Henry, G. W.\nAU - Immonen, L.\nAU - Kajatkari, P.\nAU - Lankinen, J.\nAU - Lehtinen, J.\nAU - Monira, S.\nAU - Nikbakhsh, S.\nAU - Viitanen, A.\nAU - Viuho, J.\nAU - Willamo, T.\nTA - yCat\nSO - VizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\nDP - 2017 May 01\nPG - J/AN/338/453\n4099- https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nAB - The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star.

The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&A...527A.136L, Cat. J/A+A/527/A136.

(4 data files).

\n\n\nPT - Journal Article\nTI - V694 Mon (MWC 560) spectroscopy requested\nAU - Waagen, Elizabeth O.\nAD - AA(AAVSO)\nTA - AAVSN\nSO - AAVSO Special Notice #429\nVI - 429\nDP - 2017 May 01\nPG - 1\n4099- https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nAB - The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at <lucy@astro.columbia.edu>. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details.

\n\n\nPT - Miscellaneous\nTI - Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nAU - Yan, Lin\nTA - sptz\nSO - Spitzer Proposal ID 13168\nDP - 2017 Apr 01\nPG - 13168\n4099- https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nAB - ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event.

\n\n\nPT - Thesis\nTI - Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAU - Azankpo, Severin\nAD - AA(University of Stellenbosch)\nTA - MsT\nSO - Masters thesis, University of Stellenbosch, March 2017, 120 pages\nDP - 2017 Mar 01\nPG - 2\n4099- https://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nAB - The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads.

\n\n\nPT - Report\nTI - The penumbral Moon\'s eclipse form 16 september 2016\nAU - Rotaru, Adrian\nAU - Pteancu, Mircea\nAU - Zaharia, Cristian\nAD - AA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nTA - emo6\nSO - http://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\nDP - 2016 Oct 01\n4099- https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nAB - The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon.

\n\n\nPT - Conference\nTI - Living on the edge: Adaptive Optics+Lucky Imaging\nAU - Velasco, Sergio\nAD - AA(Instituto de Astrofísica de Canarias)\nTA - iac\nSO - IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\nDP - 2016 Mar 01\nPG - 872\n4099- https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nAB - Not Available

\n\n\nPT - Book Chapter\nTI - The Diversity of Nuclear Magnetic Resonance Spectroscopy\nAU - Liu, Corey W.\nAU - Alekseyev, Viktor Y.\nAU - Allwardt, Jeffrey R.\nAU - Bankovich, Alexander J.\nAU - Cade-Menun, Barbara J.\nAU - Davis, Ronald W.\nAU - Du, Lin-Shu\nAU - Garcia, K. Christopher\nAU - Herschlag, Daniel\nAU - Khosla, Chaitan\nAU - Kraut, Daniel A.\nAU - Li, Qing\nAU - Null, Brian\nAU - Puglisi, Joseph D.\nAU - Sigala, Paul A.\nAU - Stebbins, Jonathan F.\nAU - Varani, Luca\nAD - AA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological & Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological & Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological & Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological & Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nTA - bcet\nSO - Biophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\nDP - 2009 Jan 01\nPG - 65\n4099- https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nAB - The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism.

\n\n\nPT - Conference\nTI - Time Domain Exploration with the Palomar-QUEST Sky Survey\nAU - Mahabal, Ashish A.\nAU - Drake, A. J.\nAU - Djorgovski, S. G.\nAU - Donalek, C.\nAU - Glikman, E.\nAU - Graham, M. J.\nAU - Williams, R.\nAU - Baltay, C.\nAU - Rabinowitz, D.\nAU - PQ Team Caltech\nAU - Yale\nAU - NCSA\nAU - Indiana\nAU - , . . .\nAD - AA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nTA - AAS\nSO - American Astronomical Society Meeting 210, id.21.04\nVI - 210\nDP - 2007 May 01\nPG - 21.04\n4099- https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nAB - Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system.

Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys.

We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment.

The PQ survey is partially supported by the U.S. National Science Foundation (NSF).

\n\n\nPT - Journal Article\nTI - Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nAU - ., S. N. Agbo\nAU - ., E. C. Okoroigwe\nTA - RJPh\nSO - Research Journal of Physics, vol. 1, issue 1, pp. 35-41\nVI - 1\nDP - 2007 Jan 01\nPG - 35-41\n4099- https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nAB - Not Available

\nIS - 1819-3463\n\n\nPT - Conference\nTI - Spacecraft navigation requirements\nAU - Miller, Judy L.\nAD - AA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nTA - ans\nSO - In AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\nDP - 1995 Jun 01\nPG - 390-405\n4099- https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nAB - Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy).

\n\n\nPT - Book\nTI - Applied nonlinear dynamics: analytical, computational and experimental methods\nAU - Nayfeh, Ali H.\nAU - Balachandran, Balakumar\nTA - anda\nSO - Wiley series in nonlinear science, New York; Chichester: Wiley, |c1995\nDP - 1995 Jan 01\n4099- https://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nAB - Not Available

\n\n\nPT - Preprint\nTI - Applied Conformal Field Theory\nAU - Ginsparg, Paul\nTA - arXiv\nSO - eprint arXiv:hep-th/9108028\nDP - 1988 Nov 01\nPG - hep-th/9108028\n4099- https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nAB - These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications

\n\n\nPT - Journal Article\nTI - Autonomous navigation using lunar beacons\nAU - Khatib, A. R.\nAU - Ellis, J.\nAU - French, J.\nAU - Null, G.\nAU - Yunck, T.\nAU - Wu, S.\nAD - AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nTA - aiaa\nSO - American Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\nDP - 1983 Jan 01\n4099- https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nAB - The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation.

\n\n\nPT - Miscellaneous\nTI - Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nAU - Thornton, P. E.\nAU - Thornton, M. M.\nAU - Mayer, B. W.\nAU - Wilhelmi, N.\nAU - Wei, Y.\nAU - Devarakonda, R.\nAU - Cook, R.\nTA - ddsw\nSO - Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\nDP - 2012 Apr 01\n4099- https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nAB - Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\n\n\nPT - Journal Article\nTI - Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nAU - Dhaygude, Akanksha\nAU - Desai, Shantanu\nAD - AA(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India), AB(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India ;)\nTA - EPJC\nSO - The European Physical Journal C, Volume 80, Issue 2, article id.96\nDP - 2020 Feb 01\n4099- https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\nAB - Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\n\n\n'} data_ads_publisher = {'msg': 'Retrieved 5 abstracts, starting with number 1.', 'export': "%R 2024zndo..10908474S\n%T pc2/pqdts: v2024.2\n%A Schade, Robert\n%F AA(Paderborn Center for Parallel Computing @DCM-UPB)\n%J Zenodo\n%D 04/2024\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2024zndo..10908474S\n%B Changes: improved installation mechanism for Julia spelling fixes in README.MD\n%H Zenodo\n%Y DOI: 10.5281/zenodo.10908474\n\n\n%R 2024wsp..conf...20V\n%T A modern view of former rivers on Mars.\n%A Vidmachenko, A.\n%F AA(National University of Life and Environmental Sciences of Ukraine)\n%J Proceedings of the VIII International Scientific and Practical Conference. World science priorities (February 08 – 09\n%D 02/2024\n%P 20\n%L 25\n%K Mars, riverbeds, meandering valleys, glaciers, eternal permafrost\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%I AUTHOR_HTML: Author Article;\n%U https://ui.adsabs.harvard.edu/abs/2024wsp..conf...20V\n%B Now the surface of Mars is a waterless desert, over which storms rage, raising sand and dust to a height of tens of kilometers. Under modern conditions, open bodies of water cannot exist on Mars. And water on the planet is contained either in the soil layer as permafrost, or in the form of open ice and snow; a very small amount of water is present in gaseous form in the atmosphere. The large reservoirs of water ice on Mars are the polar caps. Studies of Mars by spacecraft have shown that there is a huge amount of ice, and possibly liquid water, under the surface layer at a shallow depth. Analysis of the collected data allowed us to come to the conclusion that liquid water existed in significant quantities on the surface of Mars several billion years ago. That is, in the past, Mars had a full-fledged hydrosphere and a rather powerful atmosphere with a pressure near the surface of more than 0.4 bar. Later, the planet's climate changed. It lost much of its atmosphere and water, turning into a cold world. On the surface of Mars, there are numerous winding valleys with a long length, reminiscent of the dried-up channels of terrestrial rivers. A significant portion of the water that once flowed along currently dry riverbeds must now be under the surface of the planet. It is also possible that some channels are the result of the action of not liquid water, but a mixture of mud, ice and steam that flow only episodically. It is possible that the meandering valleys formed moving masses of glaciers. There is every reason to believe that there is still a lot of water on Mars, and it still exists in the form of permafrost. A perspective image of the Echus Chasma region suggests that liquid water was present on this part of the Martian surface up to a billion years ago. Later, the planet cooled down, the lakes froze, and glaciers formed, which 'cut' the Kasei Valles with their streams.\n%H World of Conferences\n\n\n%R 2024asal.book..204V\n%T New generation telescopes for the astronomy of the future.\n%A Vidmachenko, A.\n%F AA(National University of Life and Environmental Sciences of Ukraine)\n%J In book: Astronomical almanac\n%D 01/2024\n%P 204\n%L 209\n%K new astronomical instruments, Telescopes, telescope construction,\nastronomical research\n%I ABSTRACT: Abstract;\n%I Co-Reads: Co-Reads;\n%I AUTHOR_HTML: Author Article;\n%U https://ui.adsabs.harvard.edu/abs/2024asal.book..204V\n%B In the next few years, several new astronomical instruments are planned to be launched on Earth and in space. Each of these devices is very expensive! But many countries allocate large amounts of money for this, and plan to receive more and more recent data about the surrounding universe. Telescopes are devices for observing distant objects. The very first working telescope was created in 1608 by the Dutch optician Hans Lippersgei. The creation of the telescope was also attributed to such masters as another Dutch eyeglass maker from Middelburg, Zachary Janssen, and Jacob Mathews from the city of Alkmaar. These earliest telescopes consisted of a convex lens as an objective and a concave lens that served as an eyepiece. In 1609, Galileo Galilei significantly improved the design of the telescope, achieving a 30-fold increase in the original images. With its help, Galileo performed the first survey of the heavenly bodies. Therefore, even now, the creation of astronomical instruments, whose characteristics significantly improve previous examples of telescope construction, is considered extremely important in astronomical research. The Hubble telescope was the first to provide interesting information about the features of images of the most distant galaxies. They are significantly different from those formed relatively recently. One of the world's largest ground-based telescopes, the Giant Magellan Telescope, is under construction. It is being built in Chile and its gradual commissioning will begin in 2024. Segments of seven monolithic mirrors, with a diameter of 8.4 m each, create an optical surface with an equivalent diameter of 24.5 m. Larger will be the 30-meter telescope, which is planned to be built on the island of Hawaii, next to the two 9-meter Keck reflectors at the Mauna Kea observatory. The mirror surface of this telescope will consist of almost five hundred hexagonal segments and will reach a diameter of 30 m. It is expected to be tested in 2027. In 2014, the European Southern Observatory started the construction of the Extremely Large Telescope. In 2025, it is planned to become the most powerful optical astronomical instrument in the world, with an equivalent diameter of its mirror surface of 39 m.\n%H Kyiv\n\n\n%R 2018scrp.conf.....K\n%T Science and Computing with Raspberry Pi\n%A Kent, Brian R.\n%F AA(NRAO)\n%J Science and Computing with Raspberry Pi\n%D 07/2018\n%K single board computing, astronomy, very large array, astrophysics,\nvisualization, data science, computing, radio astronomy\n%C Copyright (c) 2018 Morgan & Claypool Publishers\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2018scrp.conf.....K\n%B The portable Raspberry Pi computing platform with the power of Linux yields an exciting exploratory tool for beginning scientific computing. Science and Computing with Raspberry Pi takes the reader through explorations in a variety of computing exercises with the physical sciences. The book guides the user through: configuring your Raspberry Pi and Linux operating system; understanding the software requirements while using the Pi for scientific computing; computing exercises in physics, astronomy, chaos theory, and machine learning.\n%H Morgan & Claypool\n\n\n%R 2023uwff.book.....R\n%T Under the weather: a future forecast for New Zealand\n%A Renwick, J. A.\n%J Under the weather: a future forecast for New Zealand\n%D 01/2023\n%I ABSTRACT: Abstract;\n%I PUB_HTML: Publisher Article;\n%U https://ui.adsabs.harvard.edu/abs/2023uwff.book.....R\n%B A forecast for New Zealand's changing climate and why it matters to our everyday lives A warmer world will change more than just our weather patterns. It will change the look of the land around us, what grows and lives on it - including us. Drawing on climate models that can travel to ice ages and hothouses of the deep past, Professor James Renwick untangles how we know exactly what the future holds and why it matters to our everyday lives. He looks at New Zealand's more frequent natural disasters, warming and increasingly acidic waters, the creep of rising sea levels, and the ways that the changing weather will affect our agriculture, lifestyle, food security and economy.Arresting, galvanizing and clear-sighted, Under the Weather is a picture of a miraculous planet in danger, a stock-take on what it means for this small country, and a reminder that the shape of our future is up to us.'--Publisher description.\n%H HarperCollins\n\n\n"} diff --git a/exportsrv/tests/unittests/stubdata/rssTest.py b/exportsrv/tests/unittests/stubdata/rssTest.py index c444be8..7da822c 100644 --- a/exportsrv/tests/unittests/stubdata/rssTest.py +++ b/exportsrv/tests/unittests/stubdata/rssTest.py @@ -1,3 +1,3 @@ # -*- coding: utf-8 -*- -data = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '\n\n\nADS (Cites/AR query)\nhttps://ui.adsabs.harvard.edu\nThe SAO/NASA ADS Abstract service provides a search system for the Astronomy and Physics literature\n\nhttp://ads.harvard.edu/figs/ads_icon_144.png\nSAO/NASA ADS\nhttps://ui.adsabs.harvard.edu\n144\n122\n\n\n\nBook reviews\nhttps://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nNot Available <P />\n\n\nFal\'ko, Vladimir: 2D Materials: maintaining editorial quality\nhttps://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nNot Available <P />\n\n\nParkin, Stuart: Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nhttps://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nNot Available <P />\n\n\nDessauges-Zavadsky, Miroslava: Millimeter Astronomy\nhttps://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nNot Available <P />\n\n\nPustilnik, M.: Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nhttps://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nNot Available <P />\n\n\nCarton, David: Resolving Gas-Phase Metallicity In Galaxies\nhttps://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nChapter 2: As part of the Bluedisk survey we analyse the radial gas-\nphase metallicity profiles of 50 late-type galaxies. We compare the\nmetallicity profiles of a sample of HI-rich galaxies against a control\nsample of HI-\'normal\' galaxies. We find the metallicity gradient of a\ngalaxy to be strongly correlated with its HI mass fraction {M}{HI}) /\n{M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity\nprofile in the outer disc than in the inner disc. These galaxies are\nfound in both the HI-rich and control samples. This contradicts a\nprevious indication that these outer drops are exclusive to HI-rich\ngalaxies. These effects are not driven by bars, although we do find some\nindication that barred galaxies have flatter metallicity profiles. By\napplying a simple analytical model we are able to account for the\nvariety of metallicity profiles that the two samples present. The\nsuccess of this model implies that the metallicity in these isolated\ngalaxies may be in a local equilibrium, regulated by star formation.\nThis insight could provide an explanation of the observed local mass-\nmetallicity relation. <P />Chapter 3 We present a method to recover the\ngas-phase metallicity gradients from integral field spectroscopic (IFS)\nobservations of barely resolved galaxies. We take a forward modelling\napproach and compare our models to the observed spatial distribution of\nemission line fluxes, accounting for the degrading effects of seeing and\nspatial binning. The method is flexible and is not limited to particular\nemission lines or instruments. We test the model through comparison to\nsynthetic observations and use downgraded observations of nearby\ngalaxies to validate this work. As a proof of concept we also apply the\nmodel to real IFS observations of high-redshift galaxies. From our\ntesting we show that the inferred metallicity gradients and central\nmetallicities are fairly insensitive to the assumptions made in the\nmodel and that they are reliably recovered for galaxies with sizes\napproximately equal to the half width at half maximum of the point-\nspread function. However, we also find that the presence of star forming\nclumps can significantly complicate the interpretation of metallicity\ngradients in moderately resolved high-redshift galaxies. Therefore we\nemphasize that care should be taken when comparing nearby well-resolved\nobservations to high-redshift observations of partially resolved\ngalaxies. <P />Chapter 4 We present gas-phase metallicity gradients for\n94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a\nnegative median metallicity gradient of (-0.043^{+0.009}_{-0.007},\ndex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies\nto be more metal-rich than their outskirts. However, there is\nsignificant scatter underlying this and we find that 10% (9) galaxies\nhave significantly positive metallicity gradients, 39% (37) have\nsignificantly negative gradients, 28% (26) have gradients consistent\nwith being flat, the remainder 23% (22) are considered to have\nunreliable gradient estimates. We find a slight trend for a more\nnegative metallicity gradient with both increasing stellar mass and\nincreasing star formation rate (SFR). However, given the potential\nredshift and size selection effects, we do not consider these trends to\nbe significant. Indeed when we normalize the SFR of our galaxies\nrelative to the main sequence, we do not observe any trend between the\nmetallicity gradient and the normalized SFR. This finding is contrary to\nother recent studies of galaxies at similar and higher redshifts. We do,\nhowever, identify a novel trend between the metallicity gradient of a\ngalaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large\nspread in observed metallicity gradients (both negative and positive\ngradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with\npositive metallicity gradients, and overall there is less scatter in the\nmetallicity gradient amongst the large galaxies. We suggest that these\nlarge (well-evolved) galaxies may be analogues of galaxies in the\npresent-day Universe, which also present a common negative metallicity\ngradient. <P />Chapter 5 The relationship between a galaxy\'s stellar\nmass and its gas-phase metallicity results from the complex interplay\nbetween star formation and the inflow and outflow of gas. Since the\ngradient of metals in galaxies is also influenced by the same processes,\nit is therefore natural to contrast the metallicity gradient with the\nmass-metallicity relation. Here we study the interrelation of the\nstellar mass, central metallicity and metallicity gradient, using a\nsample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable\nmetallicity gradient estimates. We find that typically the galaxies that\nfall below the mean mass-metallicity relation have flat or inverted\nmetallicity gradients. We quantify their relationship taking full\naccount of the covariance between the different variables and find that\nat fixed mass the central metallicity is anti-correlated with the\nmetallicity gradient. We argue that this is consistent with a scenario\nthat suppresses the central metallicity either through the inflow of\nmetal poor gas or outflow of metal enriched gas. <P />\n\n\nKohler, Susanna: A 3D View of a Supernova Remnant\nhttps://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nThe outlined regions mark the 57 knots in Tycho selected by the authors\nfor velocity measurements. Magenta regions have redshifted line-of-sight\nvelocities (moving away from us); cyan regions have blueshifted light-\nof-sight velocities (moving toward us). [Williams et al. 2017]The Tycho\nsupernova remnant was first observed in the year 1572. Nearly 450 years\nlater, astronomers have now used X-ray observations of Tycho to build\nthe first-ever 3D map of a Type Ia supernova remnant.Signs of\nExplosionsSupernova remnants are spectacular structures formed by the\nejecta of stellar explosions as they expand outwards into the\nsurrounding interstellar medium.One peculiarity of these remnants is\nthat they often exhibit asymmetries in their appearance and motion. Is\nthis because the ejecta are expanding into a nonuniform interstellar\nmedium? Or was the explosion itself asymmetric? The best way we can\nexplore this question is with detailed observations of the\nremnants.Histograms of the velocity in distribution of the knots in the\nX (green), Y (blue) and Z (red) directions (+Z is away from the\nobserver). They show no evidence for asymmetric expansion of the knots.\n[Williams et al. 2017]Enter TychoTo this end, a team of scientists led\nby Brian Williams (Space Telescope Science Institute and NASA Goddard\nSFC) has worked to map out the 3D velocities of the ejecta in the Tycho\nsupernova remnant. Tycho is a Type Ia supernova thought to be caused by\nthe thermonuclear explosion of a white dwarf in a binary system that was\ndestabilized by mass transfer from its companion.After 450 years of\nexpansion, the remnant now has the morphological appearance of a roughly\ncircular cloud of clumpy ejecta. The forward shock wave from the\nsupernova, however, is known to have twice the velocity on one side of\nthe shell as on the other.To better understand this asymmetry, Williams\nand collaborators selected a total of 57 knots in Tychos ejecta, spread\nout around the remnant. They then used 12 years of Chandra X-ray\nobservations to measure both the knots proper motion in the plane of the\nsky and their line-of-sight velocity. These two measurements were then\ncombined to build a full 3D map of the motion of the ejecta.3D\nhydrodynamical simulations of Tycho, stopped at the current epoch. These\nshow that both initially smooth (top) and initially clumpy (bottom)\nejecta models are consistent with the current observations of the\nmorphology and dynamics of Tychos ejecta. [Adapted from Williams et al.\n2017]Symmetry and ClumpsWilliams and collaborators found that the knots\nhave total velocities that range from 2400 to 6600 km/s. Unlike the\nforward shock of the supernova, Tychos ejecta display no asymmetries in\ntheir motion which suggests that the explosion itself was symmetric. The\nmore likely explanation is a density gradient in the interstellar\nmedium, which could slow the shock wave on one side of the remnant\nwithout yet affecting the motion of the clumps of ejecta.As a final\nexploration, the authors attempt to address the origin of Tychos\nclumpiness. The fact that some of Tychos ejecta knots precede its outer\nedge has raised the question of whether the ejecta started out clumpy,\nor if they began smooth and only clumped during expansion. Williams and\ncollaborators matched the morphological and dynamical data to\nsimulations, demonstrating that neither scenario can be ruled out at\nthis time.This first 3D map of a Type Ia supernova represents an\nimportant step in our ability to understand these stellar explosions.\nThe authors suggest that well be able to expand on this map in the\nfuture with additional observations from Chandra, as well as with new\ndata from future X-ray observatories that will be able to detect fainter\nemission.CitationBrian J. Williams et al 2017 ApJ 842 28.\ndoi:10.3847/1538-4357/aa7384 <P />\n\n\nGreen, D. W. E.: Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nhttps://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nA previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta\n= +0.0003 AU, solar long. = 125.841 deg). Future encounters are\npredicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July\n29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU,\n125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).\n<P />\n\n\nCasey, Andrew R.: sick: Spectroscopic inference crank\nhttps://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nsick infers astrophysical parameters from noisy observed spectra.\nPhenomena that can alter the data (e.g., redshift, continuum,\ninstrumental broadening, outlier pixels) are modeled and simultaneously\ninferred with the astrophysical parameters of interest. This package\nrelies on emcee (ascl:1303.002); it is best suited for situations where\na grid of model spectra already exists, and one would like to infer\nmodel parameters given some data. <P />\n\n\nSiltala, J.: VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nhttps://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nThe included files present the numerical data of our analysis of the BM\nCVn photometry. The data consists of differential Johnson V-band\nphotometry using the star HD 116010 as the comparison star. <P />The\nanalysis has been performed using the previously published continuous\nperiod search (CPS) method, described in detail in Lehtinen et al.,\n2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />\n\n\nWaagen, Elizabeth O.: V694 Mon (MWC 560) spectroscopy requested\nhttps://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nThe observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert\nNotice 538) has been continued, but with different requirements.\nPhotometry is no longer specifically requested on a regular basis\n(although ongoing observations that do not interfere with other\nobligations are welcome). Spectroscopy on a cadence of a week or two is\nrequested to monitor changes in the disk outflow. Investigator Adrian\nLucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University)\nhave requested spectroscopic monitoring of the broad-absorption-line\nsymbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-\nwavelength observations obtained during its recent outburst (ATel #8653,\n#8832, #8957; #10281). This system is a perfect place in which to study\nthe relationship between an accretion disk and disk winds/jets, and a\nhigh-value target for which even low-resolution spectra can be\nextraordinarily useful...Optical brightening in MWC 560 tends to predict\nhigher-velocity absorption, but sometimes jumps in absorption velocity\nalso appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242,\n187). If such a velocity jump occurs during photometric quiescence, it\nmay prompt radio observations to confirm and test the proposed outflow\norigin for recently-discovered flat-spectrum radio emission (Lucy et al.\nATel #10281)...Furthermore, volunteer spectroscopic monitoring of this\nsystem has proved useful in unpredictable ways. For example, \'amateur\'\nspectra obtained by Somogyi Péter in 2015 December demonstrated that the\nvelocity of absorption was very low only a month before an optical\noutburst peak prompted absorption troughs up to 3000 km/s, which\nconstrains very well the timing of the changes to the outflow to a\ndegree that would not have been otherwise possible. Any resolution can\nbe useful. A wavelength range that can accommodate a blueshift of at\nleast 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at\n6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra\nwith a smaller range can still be useful. Photometry could potentially\nstill be useful, but will be supplementary to medium-cadence photometry\nbeing collected by the ANS collaboration." "Spectroscopy may be uploaded\nto the ARAS database\n(http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to\nAdrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder\ncharts with sequence may be created using the AAVSO Variable Star\nPlotter (https://www.aavso.org/vsp). Photometry should be submitted to\nthe AAVSO International Database. See full Special Notice for more\ndetails. <P />\n\n\nYan, Lin: Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nhttps://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the\nfollow-up optical spectra classified this event as a TDE candidate\n(Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival\nWISE data, we discovered that its 3.4 and 4.6um fluxes have been\nsteadily rising since 2013, increased by a factor of 3.5 and 2.6\nrespectively. The last epoch data from WISE on 2016-12-12 shows that\nF01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the\nmid-IR LCs as infrared echoes from the earlier optical flare. We infer a\nconvex, dust ring with a radius of 1 pc from the central heating source.\nOur model predicts that if this event is indeed a TDE, its mid-IR LCs\nshould start to fade in next 5-12 months because it has already\nreprocessed most of the UV/optical energy from the tidal disruption.\nHowever, if this event is due to activities from an AGN, its mid-IR LCs\ncould last over a much longer time scale. We request a total of 3.2\nhours of Spitzer time to monitor the mid-IR variations in next 12\nmonths. This will provide the critical data to confirm the nature of\nthis transient event. <P />\n\n\nAzankpo, Severin: Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nhttps://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nThe African Very-long-baseline interferometry Network (AVN) is a joint\nproject between South Africa and eight partner African countries aimed\nat establishing a VLBI (Very-Long-Baseline Interferometry) capable\nnetwork of radio telescopes across the African continent. An existing\nstructure that is earmarked for this project, is a 32 m diameter antenna\nlocated in Ghana that has become obsolete due to advances in\ntelecommunication. The first phase of the conversion of this Ghana\nantenna into a radio astronomy telescope is to upgrade the antenna to\nobserve at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a\nrequired performing tolerance. The surface and pointing accuracies for a\nradio telescope are much more stringent than that of a telecommunication\nantenna. The mechanical pointing accuracy of such telescopes is\ninfluenced by factors such as mechanical alignment, structural\ndeformation, and servo drive train errors. The current research\ninvestigates the numerical simulation of the surface and pointing\naccuracies of the Ghana 32 m diameter radio astronomy telescope due to\nits structural deformation mainly influenced by gravity, wind and\nthermal loads. <P />\n\n\nRotaru, Adrian: The penumbral Moon\'s eclipse form 16 september 2016\nhttps://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nThe web page represents circumstances and photographs from the Moon\'s\npartial/penumbral eclipse from 16 September 2016 obtained from few\nvarious places in Romania (East Europe). A part of photographs give the\nmaximum phase of the Eclipse, while another give the reddened Moon. <P\n/>\n\n\nVelasco, Sergio: Living on the edge: Adaptive Optics+Lucky Imaging\nhttps://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nNot Available <P />\n\n\nLiu, Corey W.: The Diversity of Nuclear Magnetic Resonance Spectroscopy\nhttps://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nThe discovery of the physical phenomenon of Nuclear Magnetic Resonance\n(NMR) in 1946 gave rise to the spectroscopic technique that has become a\nremarkably versatile research tool. One could oversimplify NMR spectros-\ncopy by categorizing it into the two broad applications of structure\nelucidation of molecules (associated with chemistry and biology) and\nimaging (associated with medicine). But, this certainly does not do NMR\nspectroscopy justice in demonstrating its general acceptance and\nutilization across the sciences. This manuscript is not an effort to\npresent an exhaustive, or even partial review of NMR spectroscopy\napplications, but rather to provide a glimpse at the wide-ranging uses\nof NMR spectroscopy found within the confines of a single magnetic\nresonance research facility, the Stanford Magnetic Resonance Laboratory.\nIncluded here are summaries of projects involving protein structure\ndetermination, mapping of intermolecular interactions, exploring\nfundamental biological mechanisms, following compound cycling in the\nenvironmental, analysis of synthetic solid compounds, and microimaging\nof a model organism. <P />\n\n\nMahabal, Ashish A.: Time Domain Exploration with the Palomar-QUEST Sky Survey\nhttps://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nPalomar-QUEST (PQ) synoptic sky survey has now been routinely processing\ndata from driftscans in real-time. As four photometric bandpasses are\nutilized in nearly simultaneously, PQ is well suited to search for\ntransient and highly variable objects. Using a series of software\nfilters i.e. programs to select/deselect objects based on certain\ncriteria we shorten the list of candidates from the initially flagged\ncandidate transients. Such filters include looking for known asteroids,\nknown variables, as well as moving, but previously uncatalogued objects\nbased on their motion within a scan as well as between successive scans.\nSome software filters also deal with instrumental artifacts, edge\neffects, and use clustering of spurious detections around bright stars.\nDuring a typical night when we cover about 500 sq. degrees, we detect\nhundreds of asteroids, the primary contaminants in the search for\nastrophysical transients beyond our solar system. <P />Here we describe\nsome statistics based on the software filters we employ and the nature\nof the objects that seem to survive the process. We also discuss the\nusefulness of this to amateur astronomers, projects like VOEventNet, and\nother synoptic sky surveys. <P />We also present an outline of the work\nwe have started on quantifying the variability of quasars, blazars, as\nwell as various classes of Galactic sources, by combining the large\nnumber of PQ scans with other existing data sources federated in the\nVirtual Observatory environment. <P />The PQ survey is partially\nsupported by the U.S. National Science Foundation (NSF). <P />\n\n\n., S. N. Agbo: Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nhttps://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nNot Available <P />\n\n\nMiller, Judy L.: Spacecraft navigation requirements\nhttps://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nSpacecraft operation depends upon knowledge of vehicular position and,\nconsequently, navigational support has been required for all such\nsystems. Technical requirements for different mission trajectories and\norbits are addressed with consideration given to the various tradeoffs\nwhich may need to be considered. The broad spectrum of spacecraft are\nconsidered with emphasis upon those of greater military significance\n(i.e., near earth orbiting satellites). Technical requirements include,\nbut are not limited to, accuracy; physical characteristics such as\nweight and volume; support requirements such as electrical power and\nground support; and system integrity. Generic navigation suites for\nspacecraft applications are described. It is shown that operational\nspacecraft rely primarily upon ground-based tracking and computational\ncenters with little or no navigational function allocated to the\nvehicle, while technology development efforts have been and continue to\nbe directed primarily toward onboard navigation suites. The military\nsignificance of onboard navigators is shown to both improve spacecraft\nsurvivability and performance (accuracy). <P />\n\n\nNayfeh, Ali H.: Applied nonlinear dynamics: analytical, computational and experimental methods\nhttps://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nNot Available <P />\n\n\nGinsparg, Paul: Applied Conformal Field Theory\nhttps://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nThese lectures consisted of an elementary introduction to conformal\nfield theory, with some applications to statistical mechanical systems,\nand fewer to string theory. Contents: 1. Conformal theories in d\ndimensions 2. Conformal theories in 2 dimensions 3. The central charge\nand the Virasoro algebra 4. Kac determinant and unitarity 5.\nIdentication of m = 3 with the critical Ising model 6. Free bosons and\nfermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine\nKac-Moody algebras and coset constructions 10. Advanced applications <P\n/>\n\n\nKhatib, A. R.: Autonomous navigation using lunar beacons\nhttps://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nThe concept of using lunar beacon signal transmission for on-board\nnavigation for earth satellites and near-earth spacecraft is described.\nThe system would require powerful transmitters on the earth-side of the\nmoon\'s surface and black box receivers with antennae and microprocessors\nplaced on board spacecraft for autonomous navigation. Spacecraft\nnavigation requires three position and three velocity elements to\nestablish location coordinates. Two beacons could be soft-landed on the\nlunar surface at the limits of allowable separation and each would\ntransmit a wide-beam signal with cones reaching GEO heights and be\nstrong enough to be received by small antennae in near-earth orbit. The\nblack box processor would perform on-board computation with one-way\nDoppler/range data and dynamical models. Alternatively, GEO satellites\nsuch as the GPS or TDRSS spacecraft can be used with interferometric\ntechniques to provide decimeter-level accuracy for aircraft navigation.\n<P />\n\n\nThornton, P. E.: Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nhttps://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nArchived and distributed through the ORNL DAAC, the Daymet data set\nprovides gridded estimates of daily weather parameters for North\nAmerica, including daily continuous surfaces of minimum and maximum\ntemperature, precipitation occurrence and amount, humidity, shortwave\nradiation, snow water equivalent, and day length. The daily time step, 1\nkm x 1 km spatial resolution, and North American spatial extent of the\ndata set makes it a unique and valuable contribution to scientific,\nresearch, and educational communities. The literature shows that Daymet\ndata have been broadly applied to fields including hydrology,\nterrestrial vegetation growth models, carbon cycle science, and regional\nto large scale climate change analysis.\n\n\n\n'} \ No newline at end of file +data = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '\n\n\nADS (Cites/AR query)\nhttps://ui.adsabs.harvard.edu\nThe SAO/NASA ADS Abstract service provides a search system for the Astronomy and Physics literature\n\nhttp://ads.harvard.edu/figs/ads_icon_144.png\nSAO/NASA ADS\nhttps://ui.adsabs.harvard.edu\n144\n122\n\n\n\nBook reviews\nhttps://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nNot Available <P />\n\n\nFal\'ko, Vladimir: 2D Materials: maintaining editorial quality\nhttps://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nNot Available <P />\n\n\nParkin, Stuart: Obituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nhttps://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nNot Available <P />\n\n\nDessauges-Zavadsky, Miroslava: Millimeter Astronomy\nhttps://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nNot Available <P />\n\n\nPustilnik, M.: Erratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nhttps://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nNot Available <P />\n\n\nCarton, David: Resolving Gas-Phase Metallicity In Galaxies\nhttps://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nChapter 2: As part of the Bluedisk survey we analyse the radial gas-\nphase metallicity profiles of 50 late-type galaxies. We compare the\nmetallicity profiles of a sample of HI-rich galaxies against a control\nsample of HI-\'normal\' galaxies. We find the metallicity gradient of a\ngalaxy to be strongly correlated with its HI mass fraction {M}{HI}) /\n{M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity\nprofile in the outer disc than in the inner disc. These galaxies are\nfound in both the HI-rich and control samples. This contradicts a\nprevious indication that these outer drops are exclusive to HI-rich\ngalaxies. These effects are not driven by bars, although we do find some\nindication that barred galaxies have flatter metallicity profiles. By\napplying a simple analytical model we are able to account for the\nvariety of metallicity profiles that the two samples present. The\nsuccess of this model implies that the metallicity in these isolated\ngalaxies may be in a local equilibrium, regulated by star formation.\nThis insight could provide an explanation of the observed local mass-\nmetallicity relation. <P />Chapter 3 We present a method to recover the\ngas-phase metallicity gradients from integral field spectroscopic (IFS)\nobservations of barely resolved galaxies. We take a forward modelling\napproach and compare our models to the observed spatial distribution of\nemission line fluxes, accounting for the degrading effects of seeing and\nspatial binning. The method is flexible and is not limited to particular\nemission lines or instruments. We test the model through comparison to\nsynthetic observations and use downgraded observations of nearby\ngalaxies to validate this work. As a proof of concept we also apply the\nmodel to real IFS observations of high-redshift galaxies. From our\ntesting we show that the inferred metallicity gradients and central\nmetallicities are fairly insensitive to the assumptions made in the\nmodel and that they are reliably recovered for galaxies with sizes\napproximately equal to the half width at half maximum of the point-\nspread function. However, we also find that the presence of star forming\nclumps can significantly complicate the interpretation of metallicity\ngradients in moderately resolved high-redshift galaxies. Therefore we\nemphasize that care should be taken when comparing nearby well-resolved\nobservations to high-redshift observations of partially resolved\ngalaxies. <P />Chapter 4 We present gas-phase metallicity gradients for\n94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a\nnegative median metallicity gradient of (-0.043^{+0.009}_{-0.007},\ndex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies\nto be more metal-rich than their outskirts. However, there is\nsignificant scatter underlying this and we find that 10% (9) galaxies\nhave significantly positive metallicity gradients, 39% (37) have\nsignificantly negative gradients, 28% (26) have gradients consistent\nwith being flat, the remainder 23% (22) are considered to have\nunreliable gradient estimates. We find a slight trend for a more\nnegative metallicity gradient with both increasing stellar mass and\nincreasing star formation rate (SFR). However, given the potential\nredshift and size selection effects, we do not consider these trends to\nbe significant. Indeed when we normalize the SFR of our galaxies\nrelative to the main sequence, we do not observe any trend between the\nmetallicity gradient and the normalized SFR. This finding is contrary to\nother recent studies of galaxies at similar and higher redshifts. We do,\nhowever, identify a novel trend between the metallicity gradient of a\ngalaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large\nspread in observed metallicity gradients (both negative and positive\ngradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with\npositive metallicity gradients, and overall there is less scatter in the\nmetallicity gradient amongst the large galaxies. We suggest that these\nlarge (well-evolved) galaxies may be analogues of galaxies in the\npresent-day Universe, which also present a common negative metallicity\ngradient. <P />Chapter 5 The relationship between a galaxy\'s stellar\nmass and its gas-phase metallicity results from the complex interplay\nbetween star formation and the inflow and outflow of gas. Since the\ngradient of metals in galaxies is also influenced by the same processes,\nit is therefore natural to contrast the metallicity gradient with the\nmass-metallicity relation. Here we study the interrelation of the\nstellar mass, central metallicity and metallicity gradient, using a\nsample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable\nmetallicity gradient estimates. We find that typically the galaxies that\nfall below the mean mass-metallicity relation have flat or inverted\nmetallicity gradients. We quantify their relationship taking full\naccount of the covariance between the different variables and find that\nat fixed mass the central metallicity is anti-correlated with the\nmetallicity gradient. We argue that this is consistent with a scenario\nthat suppresses the central metallicity either through the inflow of\nmetal poor gas or outflow of metal enriched gas. <P />\n\n\nKohler, Susanna: A 3D View of a Supernova Remnant\nhttps://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nThe outlined regions mark the 57 knots in Tycho selected by the authors\nfor velocity measurements. Magenta regions have redshifted line-of-sight\nvelocities (moving away from us); cyan regions have blueshifted light-\nof-sight velocities (moving toward us). [Williams et al. 2017]The Tycho\nsupernova remnant was first observed in the year 1572. Nearly 450 years\nlater, astronomers have now used X-ray observations of Tycho to build\nthe first-ever 3D map of a Type Ia supernova remnant.Signs of\nExplosionsSupernova remnants are spectacular structures formed by the\nejecta of stellar explosions as they expand outwards into the\nsurrounding interstellar medium.One peculiarity of these remnants is\nthat they often exhibit asymmetries in their appearance and motion. Is\nthis because the ejecta are expanding into a nonuniform interstellar\nmedium? Or was the explosion itself asymmetric? The best way we can\nexplore this question is with detailed observations of the\nremnants.Histograms of the velocity in distribution of the knots in the\nX (green), Y (blue) and Z (red) directions (+Z is away from the\nobserver). They show no evidence for asymmetric expansion of the knots.\n[Williams et al. 2017]Enter TychoTo this end, a team of scientists led\nby Brian Williams (Space Telescope Science Institute and NASA Goddard\nSFC) has worked to map out the 3D velocities of the ejecta in the Tycho\nsupernova remnant. Tycho is a Type Ia supernova thought to be caused by\nthe thermonuclear explosion of a white dwarf in a binary system that was\ndestabilized by mass transfer from its companion.After 450 years of\nexpansion, the remnant now has the morphological appearance of a roughly\ncircular cloud of clumpy ejecta. The forward shock wave from the\nsupernova, however, is known to have twice the velocity on one side of\nthe shell as on the other.To better understand this asymmetry, Williams\nand collaborators selected a total of 57 knots in Tychos ejecta, spread\nout around the remnant. They then used 12 years of Chandra X-ray\nobservations to measure both the knots proper motion in the plane of the\nsky and their line-of-sight velocity. These two measurements were then\ncombined to build a full 3D map of the motion of the ejecta.3D\nhydrodynamical simulations of Tycho, stopped at the current epoch. These\nshow that both initially smooth (top) and initially clumpy (bottom)\nejecta models are consistent with the current observations of the\nmorphology and dynamics of Tychos ejecta. [Adapted from Williams et al.\n2017]Symmetry and ClumpsWilliams and collaborators found that the knots\nhave total velocities that range from 2400 to 6600 km/s. Unlike the\nforward shock of the supernova, Tychos ejecta display no asymmetries in\ntheir motion which suggests that the explosion itself was symmetric. The\nmore likely explanation is a density gradient in the interstellar\nmedium, which could slow the shock wave on one side of the remnant\nwithout yet affecting the motion of the clumps of ejecta.As a final\nexploration, the authors attempt to address the origin of Tychos\nclumpiness. The fact that some of Tychos ejecta knots precede its outer\nedge has raised the question of whether the ejecta started out clumpy,\nor if they began smooth and only clumped during expansion. Williams and\ncollaborators matched the morphological and dynamical data to\nsimulations, demonstrating that neither scenario can be ruled out at\nthis time.This first 3D map of a Type Ia supernova represents an\nimportant step in our ability to understand these stellar explosions.\nThe authors suggest that well be able to expand on this map in the\nfuture with additional observations from Chandra, as well as with new\ndata from future X-ray observatories that will be able to detect fainter\nemission.CitationBrian J. Williams et al 2017 ApJ 842 28.\ndoi:10.3847/1538-4357/aa7384 <P />\n\n\nGreen, D. W. E.: Potential New Meteor Shower from Comet C/2015 D4 (Borisov)\nhttps://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nA previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta\n= +0.0003 AU, solar long. = 125.841 deg). Future encounters are\npredicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July\n29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU,\n125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg).\n<P />\n\n\nCasey, Andrew R.: sick: Spectroscopic inference crank\nhttps://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nsick infers astrophysical parameters from noisy observed spectra.\nPhenomena that can alter the data (e.g., redshift, continuum,\ninstrumental broadening, outlier pixels) are modeled and simultaneously\ninferred with the astrophysical parameters of interest. This package\nrelies on emcee (ascl:1303.002); it is best suited for situations where\na grid of model spectra already exists, and one would like to infer\nmodel parameters given some data. <P />\n\n\nSiltala, J.: VizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nhttps://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nThe included files present the numerical data of our analysis of the BM\nCVn photometry. The data consists of differential Johnson V-band\nphotometry using the star HD 116010 as the comparison star. <P />The\nanalysis has been performed using the previously published continuous\nperiod search (CPS) method, described in detail in Lehtinen et al.,\n2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />\n\n\nWaagen, Elizabeth O.: V694 Mon (MWC 560) spectroscopy requested\nhttps://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nThe observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert\nNotice 538) has been continued, but with different requirements.\nPhotometry is no longer specifically requested on a regular basis\n(although ongoing observations that do not interfere with other\nobligations are welcome). Spectroscopy on a cadence of a week or two is\nrequested to monitor changes in the disk outflow. Investigator Adrian\nLucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University)\nhave requested spectroscopic monitoring of the broad-absorption-line\nsymbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-\nwavelength observations obtained during its recent outburst (ATel #8653,\n#8832, #8957; #10281). This system is a perfect place in which to study\nthe relationship between an accretion disk and disk winds/jets, and a\nhigh-value target for which even low-resolution spectra can be\nextraordinarily useful...Optical brightening in MWC 560 tends to predict\nhigher-velocity absorption, but sometimes jumps in absorption velocity\nalso appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242,\n187). If such a velocity jump occurs during photometric quiescence, it\nmay prompt radio observations to confirm and test the proposed outflow\norigin for recently-discovered flat-spectrum radio emission (Lucy et al.\nATel #10281)...Furthermore, volunteer spectroscopic monitoring of this\nsystem has proved useful in unpredictable ways. For example, \'amateur\'\nspectra obtained by Somogyi Péter in 2015 December demonstrated that the\nvelocity of absorption was very low only a month before an optical\noutburst peak prompted absorption troughs up to 3000 km/s, which\nconstrains very well the timing of the changes to the outflow to a\ndegree that would not have been otherwise possible. Any resolution can\nbe useful. A wavelength range that can accommodate a blueshift of at\nleast 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at\n6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra\nwith a smaller range can still be useful. Photometry could potentially\nstill be useful, but will be supplementary to medium-cadence photometry\nbeing collected by the ANS collaboration." "Spectroscopy may be uploaded\nto the ARAS database\n(http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to\nAdrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder\ncharts with sequence may be created using the AAVSO Variable Star\nPlotter (https://www.aavso.org/vsp). Photometry should be submitted to\nthe AAVSO International Database. See full Special Notice for more\ndetails. <P />\n\n\nYan, Lin: Confirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nhttps://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the\nfollow-up optical spectra classified this event as a TDE candidate\n(Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival\nWISE data, we discovered that its 3.4 and 4.6um fluxes have been\nsteadily rising since 2013, increased by a factor of 3.5 and 2.6\nrespectively. The last epoch data from WISE on 2016-12-12 shows that\nF01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the\nmid-IR LCs as infrared echoes from the earlier optical flare. We infer a\nconvex, dust ring with a radius of 1 pc from the central heating source.\nOur model predicts that if this event is indeed a TDE, its mid-IR LCs\nshould start to fade in next 5-12 months because it has already\nreprocessed most of the UV/optical energy from the tidal disruption.\nHowever, if this event is due to activities from an AGN, its mid-IR LCs\ncould last over a much longer time scale. We request a total of 3.2\nhours of Spitzer time to monitor the mid-IR variations in next 12\nmonths. This will provide the critical data to confirm the nature of\nthis transient event. <P />\n\n\nAzankpo, Severin: Surface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nhttps://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nThe African Very-long-baseline interferometry Network (AVN) is a joint\nproject between South Africa and eight partner African countries aimed\nat establishing a VLBI (Very-Long-Baseline Interferometry) capable\nnetwork of radio telescopes across the African continent. An existing\nstructure that is earmarked for this project, is a 32 m diameter antenna\nlocated in Ghana that has become obsolete due to advances in\ntelecommunication. The first phase of the conversion of this Ghana\nantenna into a radio astronomy telescope is to upgrade the antenna to\nobserve at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a\nrequired performing tolerance. The surface and pointing accuracies for a\nradio telescope are much more stringent than that of a telecommunication\nantenna. The mechanical pointing accuracy of such telescopes is\ninfluenced by factors such as mechanical alignment, structural\ndeformation, and servo drive train errors. The current research\ninvestigates the numerical simulation of the surface and pointing\naccuracies of the Ghana 32 m diameter radio astronomy telescope due to\nits structural deformation mainly influenced by gravity, wind and\nthermal loads. <P />\n\n\nRotaru, Adrian: The penumbral Moon\'s eclipse form 16 september 2016\nhttps://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nThe web page represents circumstances and photographs from the Moon\'s\npartial/penumbral eclipse from 16 September 2016 obtained from few\nvarious places in Romania (East Europe). A part of photographs give the\nmaximum phase of the Eclipse, while another give the reddened Moon. <P\n/>\n\n\nVelasco, Sergio: Living on the edge: Adaptive Optics+Lucky Imaging\nhttps://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nNot Available <P />\n\n\nLiu, Corey W.: The Diversity of Nuclear Magnetic Resonance Spectroscopy\nhttps://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nThe discovery of the physical phenomenon of Nuclear Magnetic Resonance\n(NMR) in 1946 gave rise to the spectroscopic technique that has become a\nremarkably versatile research tool. One could oversimplify NMR spectros-\ncopy by categorizing it into the two broad applications of structure\nelucidation of molecules (associated with chemistry and biology) and\nimaging (associated with medicine). But, this certainly does not do NMR\nspectroscopy justice in demonstrating its general acceptance and\nutilization across the sciences. This manuscript is not an effort to\npresent an exhaustive, or even partial review of NMR spectroscopy\napplications, but rather to provide a glimpse at the wide-ranging uses\nof NMR spectroscopy found within the confines of a single magnetic\nresonance research facility, the Stanford Magnetic Resonance Laboratory.\nIncluded here are summaries of projects involving protein structure\ndetermination, mapping of intermolecular interactions, exploring\nfundamental biological mechanisms, following compound cycling in the\nenvironmental, analysis of synthetic solid compounds, and microimaging\nof a model organism. <P />\n\n\nMahabal, Ashish A.: Time Domain Exploration with the Palomar-QUEST Sky Survey\nhttps://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nPalomar-QUEST (PQ) synoptic sky survey has now been routinely processing\ndata from driftscans in real-time. As four photometric bandpasses are\nutilized in nearly simultaneously, PQ is well suited to search for\ntransient and highly variable objects. Using a series of software\nfilters i.e. programs to select/deselect objects based on certain\ncriteria we shorten the list of candidates from the initially flagged\ncandidate transients. Such filters include looking for known asteroids,\nknown variables, as well as moving, but previously uncatalogued objects\nbased on their motion within a scan as well as between successive scans.\nSome software filters also deal with instrumental artifacts, edge\neffects, and use clustering of spurious detections around bright stars.\nDuring a typical night when we cover about 500 sq. degrees, we detect\nhundreds of asteroids, the primary contaminants in the search for\nastrophysical transients beyond our solar system. <P />Here we describe\nsome statistics based on the software filters we employ and the nature\nof the objects that seem to survive the process. We also discuss the\nusefulness of this to amateur astronomers, projects like VOEventNet, and\nother synoptic sky surveys. <P />We also present an outline of the work\nwe have started on quantifying the variability of quasars, blazars, as\nwell as various classes of Galactic sources, by combining the large\nnumber of PQ scans with other existing data sources federated in the\nVirtual Observatory environment. <P />The PQ survey is partially\nsupported by the U.S. National Science Foundation (NSF). <P />\n\n\n., S. N. Agbo: Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\nhttps://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nNot Available <P />\n\n\nMiller, Judy L.: Spacecraft navigation requirements\nhttps://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nSpacecraft operation depends upon knowledge of vehicular position and,\nconsequently, navigational support has been required for all such\nsystems. Technical requirements for different mission trajectories and\norbits are addressed with consideration given to the various tradeoffs\nwhich may need to be considered. The broad spectrum of spacecraft are\nconsidered with emphasis upon those of greater military significance\n(i.e., near earth orbiting satellites). Technical requirements include,\nbut are not limited to, accuracy; physical characteristics such as\nweight and volume; support requirements such as electrical power and\nground support; and system integrity. Generic navigation suites for\nspacecraft applications are described. It is shown that operational\nspacecraft rely primarily upon ground-based tracking and computational\ncenters with little or no navigational function allocated to the\nvehicle, while technology development efforts have been and continue to\nbe directed primarily toward onboard navigation suites. The military\nsignificance of onboard navigators is shown to both improve spacecraft\nsurvivability and performance (accuracy). <P />\n\n\nNayfeh, Ali H.: Applied nonlinear dynamics: analytical, computational and experimental methods\nhttps://ui.adsabs.harvard.edu/abs/1995anda.book.....N\nNot Available <P />\n\n\nGinsparg, Paul: Applied Conformal Field Theory\nhttps://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\nThese lectures consisted of an elementary introduction to conformal\nfield theory, with some applications to statistical mechanical systems,\nand fewer to string theory. Contents: 1. Conformal theories in d\ndimensions 2. Conformal theories in 2 dimensions 3. The central charge\nand the Virasoro algebra 4. Kac determinant and unitarity 5.\nIdentication of m = 3 with the critical Ising model 6. Free bosons and\nfermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine\nKac-Moody algebras and coset constructions 10. Advanced applications <P\n/>\n\n\nKhatib, A. R.: Autonomous navigation using lunar beacons\nhttps://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nThe concept of using lunar beacon signal transmission for on-board\nnavigation for earth satellites and near-earth spacecraft is described.\nThe system would require powerful transmitters on the earth-side of the\nmoon\'s surface and black box receivers with antennae and microprocessors\nplaced on board spacecraft for autonomous navigation. Spacecraft\nnavigation requires three position and three velocity elements to\nestablish location coordinates. Two beacons could be soft-landed on the\nlunar surface at the limits of allowable separation and each would\ntransmit a wide-beam signal with cones reaching GEO heights and be\nstrong enough to be received by small antennae in near-earth orbit. The\nblack box processor would perform on-board computation with one-way\nDoppler/range data and dynamical models. Alternatively, GEO satellites\nsuch as the GPS or TDRSS spacecraft can be used with interferometric\ntechniques to provide decimeter-level accuracy for aircraft navigation.\n<P />\n\n\nThornton, P. E.: Daymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nhttps://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\nArchived and distributed through the ORNL DAAC, the Daymet data set\nprovides gridded estimates of daily weather parameters for North\nAmerica, including daily continuous surfaces of minimum and maximum\ntemperature, precipitation occurrence and amount, humidity, shortwave\nradiation, snow water equivalent, and day length. The daily time step, 1\nkm x 1 km spatial resolution, and North American spatial extent of the\ndata set makes it a unique and valuable contribution to scientific,\nresearch, and educational communities. The literature shows that Daymet\ndata have been broadly applied to fields including hydrology,\nterrestrial vegetation growth models, carbon cycle science, and regional\nto large scale climate change analysis.\n\n\nDhaygude, Akanksha: Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nhttps://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\nRecently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl\nradioactive decay data from measurements at the Physikalisch-Technische\nBundesanstalt (PTB), in order to verify the claims by Sturrock and\ncollaborators of an influence on beta-decay rates measured at Brookhaven\nNational Lab (BNL) due to the rotation-induced modulation of the solar\nneutrino flux. Their analysis excluded any sinusoidal modulations in the\nfrequency range from 0.2 to 20/year. We carry out an independent\nanalysis of the same PTB and BNL data, using the generalized\nLomb–Scargle periodogram to look for any statistically significant peaks\nin the range from 0 to 14 per year, and by evaluating the significance\nof every peak using multiple methods. Our results for the PTB data are\nin agreement with those by Pomme et al. For BNL data, we do find peaks\nat some of the same frequencies as Sturrock et al., but the significance\nis much lower. All our analysis codes and datasets have been made\npublicly available.\n\n\n\n'} \ No newline at end of file diff --git a/exportsrv/tests/unittests/stubdata/solrdata.py b/exportsrv/tests/unittests/stubdata/solrdata.py index 047407a..437f6a6 100644 --- a/exportsrv/tests/unittests/stubdata/solrdata.py +++ b/exportsrv/tests/unittests/stubdata/solrdata.py @@ -26,7 +26,7 @@ }, u'response': { u'start': 0, - u'numFound': 23, + u'numFound': 24, u'docs': [ { u'read_count': 0, @@ -542,6 +542,43 @@ u'aff': [u'-', u'-', u'-', u'-', u'-', u'-', u'-'], u'num_references': 0 }, + { + "bibcode":"2020EPJC...80...96D", + "abstract":"Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.", + "aff":["Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India", + "Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India ;"], + "author":["Dhaygude, Akanksha", + "Desai, Shantanu"], + "bibstem":["EPJC", + "EPJC...80"], + "copyright":"© The Author(s) 2020", + "doctype":"article", + "doi":["10.1140/epjc/s10052-020-7683-6", + "10.48550/arXiv.1912.06970"], + "identifier":["2019arXiv191206970D", + "10.48550/arXiv.1912.06970", + "10.1140/epjc/s10052-020-7683-6", + "2020EPJC...80...96D", + "arXiv:1912.06970"], + "keyword":["Astrophysics - High Energy Astrophysical Phenomena", + "Astrophysics - Instrumentation and Methods for Astrophysics", + "Nuclear Experiment"], + "pub":"European Physical Journal C", + "pub_raw":"The European Physical Journal C, Volume 80, Issue 2, article id.96", + "pubdate":"2020-02-00", + "title":["Generalized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL"], + "year":"2020", + "read_count":168, + "esources":["EPRINT_HTML", + "EPRINT_PDF", + "PUB_HTML"], + "property":["ARTICLE", + "EPRINT_OPENACCESS", + "ESOURCE", + "OPENACCESS", + "PUB_OPENACCESS", + "REFEREED"] + }, ] } } diff --git a/exportsrv/tests/unittests/stubdata/voTableTest.py b/exportsrv/tests/unittests/stubdata/voTableTest.py index edf9c58..fe010f8 100644 --- a/exportsrv/tests/unittests/stubdata/voTableTest.py +++ b/exportsrv/tests/unittests/stubdata/voTableTest.py @@ -1,3 +1,3 @@ # -*- coding: utf-8 -*- -data = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '\n\n\n\n Results generated from the NASA Astrophysics Data System: https://ui.adsabs.harvard.edu\n For more information and support please contact ads@cfa.harvard.edu\n\n\n\n\n ADS Search Results.\n Selected and retrieved 23 records.\n\n\nThe bibcode identifier for the record\n\n\nTitle of the paper\n\n\nList of authors\n\n\nPublication infromation\n\n\nPublication Date\n\n\nResource URL\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n
2018Wthr...73Q..35.Book reviews\nWeather, vol. 73, issue 1, pp. 35-352018-01-1https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.
2018TDM.....5a0201F2D Materials: maintaining editorial qualityFal\'ko, Vladimir; Thomas, Ceri-Wyn2D Materials, Volume 5, Issue 1, article id. 010201 (2018).2018-01-1https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F
2018Spin....877001PObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting EditorParkin, Stuart; Chantrell, Roy; Chang, Ching-RaySpin, Volume 8, Issue 4, id. 18770012018-01-1https://ui.adsabs.harvard.edu/abs/2018Spin....877001P
2018SAAS...38.....DMillimeter AstronomyDessauges-Zavadsky, Miroslava; Pfenniger, DanielMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 20182018-01-1https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D
2018PhRvL.120b9901PErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]Pustilnik, M.; van Heck, B.; Lutchyn, R. M.; Glazman, L. I.Physical Review Letters, Volume 120, Issue 2, id.0299012018-01-1https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P
2017PhDT........14CResolving Gas-Phase Metallicity In GalaxiesCarton, DavidPhD Thesis, Leiden University, 20172017-06-1https://ui.adsabs.harvard.edu/abs/2017PhDT........14C
2017nova.pres.2388KA 3D View of a Supernova RemnantKohler, SusannaAAS Nova Highlight, 14 Jun 2017, id.23882017-06-1https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K
2017CBET.4403....2GPotential New Meteor Shower from Comet C/2015 D4 (Borisov)Green, D. W. E.Central Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.2017-06-1https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G
2017ascl.soft06009Csick: Spectroscopic inference crankCasey, Andrew R.Astrophysics Source Code Library, record ascl:1706.0092017-06-1https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C
2017yCat.113380453SVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)Siltala, J.; Jetsu, L.; Hackman, T.; Henry, G. W.; Immonen, L.; Kajatkari, P.; Lankinen, J.; Lehtinen, J.; Monira, S.; Nikbakhsh, S.; Viitanen, A.; Viuho, J.; Willamo, T.VizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S2017-05-1https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S
2017AAVSN.429....1WV694 Mon (MWC 560) spectroscopy requestedWaagen, Elizabeth O.AAVSO Special Notice #4292017-05-1https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W
2017sptz.prop13168YConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light CurvesYan, LinSpitzer Proposal ID 131682017-04-1https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y
2017MsT..........2ASurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy TelescopeAzankpo, SeverinMasters thesis, University of Stellenbosch, March 2017, 120 pages2017-03-1https://ui.adsabs.harvard.edu/abs/2017MsT..........2A
2016emo6.rept.....RThe penumbral Moon\'s eclipse form 16 september 2016Rotaru, Adrian; Pteancu, Mircea; Zaharia, Cristianhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)2016-10-1https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R
2016iac..talk..872VLiving on the edge: Adaptive Optics+Lucky ImagingVelasco, SergioIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 8722016-03-1https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V
2009bcet.book...65LThe Diversity of Nuclear Magnetic Resonance SpectroscopyLiu, Corey W.; Alekseyev, Viktor Y.; Allwardt, Jeffrey R.; Bankovich, Alexander J.; Cade-Menun, Barbara J.; Davis, Ronald W.; Du, Lin-Shu; Garcia, K. Christopher; Herschlag, Daniel; Khosla, Chaitan; Kraut, Daniel A.; Li, Qing; Null, Brian; Puglisi, Joseph D.; Sigala, Paul A.; Stebbins, Jonathan F.; Varani, LucaBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 652009-01-1https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L
2007AAS...210.2104MTime Domain Exploration with the Palomar-QUEST Sky SurveyMahabal, Ashish A.; Drake, A. J.; Djorgovski, S. G.; Donalek, C.; Glikman, E.; Graham, M. J.; Williams, R.; Baltay, C.; Rabinowitz, D.; PQ Team Caltech; Yale; NCSA; Indiana; , . . .American Astronomical Society Meeting 210, id.21.042007-05-1https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M
2007RJPh....1...35.Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater., S. N. Agbo; ., E. C. OkoroigweResearch Journal of Physics, vol. 1, issue 1, pp. 35-412007-01-1https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.
1995ans..agar..390MSpacecraft navigation requirementsMiller, Judy L.In AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)1995-06-1https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M
1995anda.book.....NApplied nonlinear dynamics: analytical, computational and experimental methodsNayfeh, Ali H.; Balachandran, BalakumarWiley series in nonlinear science, New York; Chichester: Wiley, |c19951995-01-1https://ui.adsabs.harvard.edu/abs/1995anda.book.....N
1991hep.th....8028GApplied Conformal Field TheoryGinsparg, Pauleprint arXiv:hep-th/91080281988-11-1https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G
1983aiaa.meetY....KAutonomous navigation using lunar beaconsKhatib, A. R.; Ellis, J.; French, J.; Null, G.; Yunck, T.; Wu, S.American Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.1983-01-1https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K
2012ddsw.rept.....TDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008Thornton, P. E.; Thornton, M. M.; Mayer, B. W.; Wilhelmi, N.; Wei, Y.; Devarakonda, R.; Cook, R.Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)2012-04-1https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T
\n\n'} \ No newline at end of file +data = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '\n\n\n\n Results generated from the NASA Astrophysics Data System: https://ui.adsabs.harvard.edu\n For more information and support please contact ads@cfa.harvard.edu\n\n\n\n\n ADS Search Results.\n Selected and retrieved 24 records.\n\n\nThe bibcode identifier for the record\n\n\nTitle of the paper\n\n\nList of authors\n\n\nPublication infromation\n\n\nPublication Date\n\n\nResource URL\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n\n
2018Wthr...73Q..35.Book reviews\nWeather, vol. 73, issue 1, pp. 35-352018-01-1https://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.
2018TDM.....5a0201F2D Materials: maintaining editorial qualityFal\'ko, Vladimir; Thomas, Ceri-Wyn2D Materials, Volume 5, Issue 1, article id. 010201 (2018).2018-01-1https://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F
2018Spin....877001PObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting EditorParkin, Stuart; Chantrell, Roy; Chang, Ching-RaySpin, Volume 8, Issue 4, id. 18770012018-01-1https://ui.adsabs.harvard.edu/abs/2018Spin....877001P
2018SAAS...38.....DMillimeter AstronomyDessauges-Zavadsky, Miroslava; Pfenniger, DanielMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 20182018-01-1https://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D
2018PhRvL.120b9901PErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]Pustilnik, M.; van Heck, B.; Lutchyn, R. M.; Glazman, L. I.Physical Review Letters, Volume 120, Issue 2, id.0299012018-01-1https://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P
2017PhDT........14CResolving Gas-Phase Metallicity In GalaxiesCarton, DavidPhD Thesis, Leiden University, 20172017-06-1https://ui.adsabs.harvard.edu/abs/2017PhDT........14C
2017nova.pres.2388KA 3D View of a Supernova RemnantKohler, SusannaAAS Nova Highlight, 14 Jun 2017, id.23882017-06-1https://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K
2017CBET.4403....2GPotential New Meteor Shower from Comet C/2015 D4 (Borisov)Green, D. W. E.Central Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.2017-06-1https://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G
2017ascl.soft06009Csick: Spectroscopic inference crankCasey, Andrew R.Astrophysics Source Code Library, record ascl:1706.0092017-06-1https://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C
2017yCat.113380453SVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)Siltala, J.; Jetsu, L.; Hackman, T.; Henry, G. W.; Immonen, L.; Kajatkari, P.; Lankinen, J.; Lehtinen, J.; Monira, S.; Nikbakhsh, S.; Viitanen, A.; Viuho, J.; Willamo, T.VizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S2017-05-1https://ui.adsabs.harvard.edu/abs/2017yCat.113380453S
2017AAVSN.429....1WV694 Mon (MWC 560) spectroscopy requestedWaagen, Elizabeth O.AAVSO Special Notice #4292017-05-1https://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W
2017sptz.prop13168YConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light CurvesYan, LinSpitzer Proposal ID 131682017-04-1https://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y
2017MsT..........2ASurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy TelescopeAzankpo, SeverinMasters thesis, University of Stellenbosch, March 2017, 120 pages2017-03-1https://ui.adsabs.harvard.edu/abs/2017MsT..........2A
2016emo6.rept.....RThe penumbral Moon\'s eclipse form 16 september 2016Rotaru, Adrian; Pteancu, Mircea; Zaharia, Cristianhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)2016-10-1https://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R
2016iac..talk..872VLiving on the edge: Adaptive Optics+Lucky ImagingVelasco, SergioIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 8722016-03-1https://ui.adsabs.harvard.edu/abs/2016iac..talk..872V
2009bcet.book...65LThe Diversity of Nuclear Magnetic Resonance SpectroscopyLiu, Corey W.; Alekseyev, Viktor Y.; Allwardt, Jeffrey R.; Bankovich, Alexander J.; Cade-Menun, Barbara J.; Davis, Ronald W.; Du, Lin-Shu; Garcia, K. Christopher; Herschlag, Daniel; Khosla, Chaitan; Kraut, Daniel A.; Li, Qing; Null, Brian; Puglisi, Joseph D.; Sigala, Paul A.; Stebbins, Jonathan F.; Varani, LucaBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 652009-01-1https://ui.adsabs.harvard.edu/abs/2009bcet.book...65L
2007AAS...210.2104MTime Domain Exploration with the Palomar-QUEST Sky SurveyMahabal, Ashish A.; Drake, A. J.; Djorgovski, S. G.; Donalek, C.; Glikman, E.; Graham, M. J.; Williams, R.; Baltay, C.; Rabinowitz, D.; PQ Team Caltech; Yale; NCSA; Indiana; , . . .American Astronomical Society Meeting 210, id.21.042007-05-1https://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M
2007RJPh....1...35.Analysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater., S. N. Agbo; ., E. C. OkoroigweResearch Journal of Physics, vol. 1, issue 1, pp. 35-412007-01-1https://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.
1995ans..agar..390MSpacecraft navigation requirementsMiller, Judy L.In AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)1995-06-1https://ui.adsabs.harvard.edu/abs/1995ans..agar..390M
1995anda.book.....NApplied nonlinear dynamics: analytical, computational and experimental methodsNayfeh, Ali H.; Balachandran, BalakumarWiley series in nonlinear science, New York; Chichester: Wiley, |c19951995-01-1https://ui.adsabs.harvard.edu/abs/1995anda.book.....N
1991hep.th....8028GApplied Conformal Field TheoryGinsparg, Pauleprint arXiv:hep-th/91080281988-11-1https://ui.adsabs.harvard.edu/abs/1991hep.th....8028G
1983aiaa.meetY....KAutonomous navigation using lunar beaconsKhatib, A. R.; Ellis, J.; French, J.; Null, G.; Yunck, T.; Wu, S.American Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.1983-01-1https://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K
2012ddsw.rept.....TDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008Thornton, P. E.; Thornton, M. M.; Mayer, B. W.; Wilhelmi, N.; Wei, Y.; Devarakonda, R.; Cook, R.Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)2012-04-1https://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T
2020EPJC...80...96DGeneralized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNLDhaygude, Akanksha; Desai, ShantanuThe European Physical Journal C, Volume 80, Issue 2, article id.962020-02-1https://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D
\n\n'} \ No newline at end of file diff --git a/exportsrv/tests/unittests/stubdata/xmlTest.py b/exportsrv/tests/unittests/stubdata/xmlTest.py index 0954cfa..235cf07 100755 --- a/exportsrv/tests/unittests/stubdata/xmlTest.py +++ b/exportsrv/tests/unittests/stubdata/xmlTest.py @@ -1,19 +1,19 @@ # -*- coding: utf-8 -*- -data_dublin_core = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '\n\n\n2018Wthr...73Q..35.\nBook reviews\nWeather, vol. 73, issue 1, pp. 35-35\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nNot Available <P />\ndoi:10.1002/wea.3072\n\n\n\n2018TDM.....5a0201F\n2D Materials: maintaining editorial quality\nFal\'ko, Vladimir\nThomas, Ceri-Wyn\n2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nNot Available <P />\ndoi:10.1088/2053-1583/aa9403\n\n\n\n2018Spin....877001P\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nParkin, Stuart\nChantrell, Roy\nChang, Ching-Ray\nSpin, Volume 8, Issue 4, id. 1877001\n2018-01-01\n(c) 2018: World Scientific Publishing Company\nhttps://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nNot Available <P />\ndoi:10.1142/S2010324718770015\n\n\n\n2018SAAS...38.....D\nMillimeter Astronomy\nDessauges-Zavadsky, Miroslava\nPfenniger, Daniel\nMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\n2018-01-01\nPhysics\n(c) 2018: Springer-Verlag GmbH Germany, part of Springer Nature\nhttps://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nNot Available <P />\ndoi:10.1007/978-3-662-57546-8\n\n\n\n2018PhRvL.120b9901P\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nPustilnik, M.\nvan Heck, B.\nLutchyn, R. M.\nGlazman, L. I.\nPhysical Review Letters, Volume 120, Issue 2, id.029901\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nNot Available <P />\ndoi:10.1103/PhysRevLett.120.029901\n\n\n\n2017PhDT........14C\nResolving Gas-Phase Metallicity In Galaxies\nCarton, David\nPhD Thesis, Leiden University, 2017\n2017-06-01\ngalaxies: evolution, galaxies: abundances, galaxies: ISM\nhttps://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nChapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation. <P />Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies. <P />Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient. <P />Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas. <P />\ndoi:10.5281/zenodo.581221\n\n\n\n2017nova.pres.2388K\nA 3D View of a Supernova Remnant\nKohler, Susanna\nAAS Nova Highlight, 14 Jun 2017, id.2388\n2017-06-01\nFeatures, Highlights, interstellar medium, stellar evolution, supernova remnant, supernovae, white dwarfs\nhttps://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nThe outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384 <P />\n\n\n\n2017CBET.4403....2G\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\nGreen, D. W. E.\nCentral Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\n2017-06-01\nhttps://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nA previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg). <P />\n\n\n\n2017ascl.soft06009C\nsick: Spectroscopic inference crank\nCasey, Andrew R.\nAstrophysics Source Code Library, record ascl:1706.009\n2017-06-01\nSoftware\nhttps://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nsick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data. <P />\n\n\n\n2017yCat.113380453S\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nSiltala, J.\nJetsu, L.\nHackman, T.\nHenry, G. W.\nImmonen, L.\nKajatkari, P.\nLankinen, J.\nLehtinen, J.\nMonira, S.\nNikbakhsh, S.\nViitanen, A.\nViuho, J.\nWillamo, T.\nVizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\n2017-05-01\nStars: variable\nhttps://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nThe included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star. <P />The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />\n\n\n\n2017AAVSN.429....1W\nV694 Mon (MWC 560) spectroscopy requested\nWaagen, Elizabeth O.\nAAVSO Special Notice #429\n2017-05-01\nastronomical databases: miscellaneous, binaries: symbiotic, stars: individual (V694 Mon, MWC 560)\n(C) AAVSO 2017\nhttps://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nThe observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details. <P />\n\n\n\n2017sptz.prop13168Y\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nYan, Lin\nSpitzer Proposal ID 13168\n2017-04-01\nhttps://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event. <P />\n\n\n\n2017MsT..........2A\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAzankpo, Severin\nMasters thesis, University of Stellenbosch, March 2017, 120 pages\n2017-03-01\nhttps://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nThe African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads. <P />\n\n\n\n2016emo6.rept.....R\nThe penumbral Moon\'s eclipse form 16 september 2016\nRotaru, Adrian\nPteancu, Mircea\nZaharia, Cristian\nhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\n2016-10-01\nTHE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY\nhttps://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nThe web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon. <P />\n\n\n\n2016iac..talk..872V\nLiving on the edge: Adaptive Optics+Lucky Imaging\nVelasco, Sergio\nIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\n2016-03-01\nhttps://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nNot Available <P />\n\n\n\n2009bcet.book...65L\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\nLiu, Corey W.\nAlekseyev, Viktor Y.\nAllwardt, Jeffrey R.\nBankovich, Alexander J.\nCade-Menun, Barbara J.\nDavis, Ronald W.\nDu, Lin-Shu\nGarcia, K. Christopher\nHerschlag, Daniel\nKhosla, Chaitan\nKraut, Daniel A.\nLi, Qing\nNull, Brian\nPuglisi, Joseph D.\nSigala, Paul A.\nStebbins, Jonathan F.\nVarani, Luca\nBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\n2009-01-01\nPhysics\n(c) 2009: Springer Netherlands\nhttps://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nThe discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism. <P />\ndoi:10.1007/978-90-481-2368-1_5\n\n\n\n2007AAS...210.2104M\nTime Domain Exploration with the Palomar-QUEST Sky Survey\nMahabal, Ashish A.\nDrake, A. J.\nDjorgovski, S. G.\nDonalek, C.\nGlikman, E.\nGraham, M. J.\nWilliams, R.\nBaltay, C.\nRabinowitz, D.\nPQ Team Caltech\nYale\nNCSA\nIndiana\n, . . .\nAmerican Astronomical Society Meeting 210, id.21.04\n2007-05-01\nhttps://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nPalomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system. <P />Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys. <P />We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment. <P />The PQ survey is partially supported by the U.S. National Science Foundation (NSF). <P />\n\n\n\n2007RJPh....1...35.\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n., S. N. Agbo\n., E. C. Okoroigwe\nResearch Journal of Physics, vol. 1, issue 1, pp. 35-41\n2007-01-01\nhttps://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nNot Available <P />\ndoi:10.3923/rjp.2007.35.41\n\n\n\n1995ans..agar..390M\nSpacecraft navigation requirements\nMiller, Judy L.\nIn AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\n1995-06-01\nEarth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space Navigation, Spacecraft Trajectories, Support Systems, Technology Assessment, Technology Utilization, Ascent Trajectories, Reentry Trajectories, Spacecraft, Spacecraft Performance, Spacecraft Survivability, Tradeoffs, Weight (Mass), Space Communications, Spacecraft Communications, Command and Tracking\nhttps://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nSpacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy). <P />\n\n\n\n1995anda.book.....N\nApplied nonlinear dynamics: analytical, computational and experimental methods\nNayfeh, Ali H.\nBalachandran, Balakumar\nWiley series in nonlinear science, New York; Chichester: Wiley, |c1995\n1995-01-01\nhttps://ui.adsabs.harvard.edu/abs/1995anda.book.....N\ncitations:118\nNot Available <P />\n\n\n\n1991hep.th....8028G\nApplied Conformal Field Theory\nGinsparg, Paul\neprint arXiv:hep-th/9108028\n1988-11-01\nHigh Energy Physics - Theory\nhttps://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\ncitations:190\nThese lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications <P />\n\n\n\n1983aiaa.meetY....K\nAutonomous navigation using lunar beacons\nKhatib, A. R.\nEllis, J.\nFrench, J.\nNull, G.\nYunck, T.\nWu, S.\nAmerican Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\n1983-01-01\nArtificial Satellites, Autonomous Navigation, Earth-Moon System, Lunar Communication, Radio Beacons, Radio Navigation, Space Navigation, Doppler Navigation, Least Squares Method, Orbit Calculation, Space Communications, Spacecraft Communications, Command and Tracking\nhttps://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nThe concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation. <P />\n\n\n\n2012ddsw.rept.....T\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nThornton, P. E.\nThornton, M. M.\nMayer, B. W.\nWilhelmi, N.\nWei, Y.\nDevarakonda, R.\nCook, R.\nOak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\n2012-04-01\nDaymet\nOak Ridge National Laboratory\nhttps://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\ncitations:51\nArchived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\ndoi:10.3334/ORNLDAAC/1219\n\n\n'} +data_dublin_core = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '\n\n\n2018Wthr...73Q..35.\nBook reviews\nWeather, vol. 73, issue 1, pp. 35-35\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nNot Available <P />\ndoi:10.1002/wea.3072\n\n\n\n2018TDM.....5a0201F\n2D Materials: maintaining editorial quality\nFal\'ko, Vladimir\nThomas, Ceri-Wyn\n2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nNot Available <P />\ndoi:10.1088/2053-1583/aa9403\n\n\n\n2018Spin....877001P\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nParkin, Stuart\nChantrell, Roy\nChang, Ching-Ray\nSpin, Volume 8, Issue 4, id. 1877001\n2018-01-01\n(c) 2018: World Scientific Publishing Company\nhttps://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nNot Available <P />\ndoi:10.1142/S2010324718770015\n\n\n\n2018SAAS...38.....D\nMillimeter Astronomy\nDessauges-Zavadsky, Miroslava\nPfenniger, Daniel\nMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\n2018-01-01\nPhysics\n(c) 2018: Springer-Verlag GmbH Germany, part of Springer Nature\nhttps://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nNot Available <P />\ndoi:10.1007/978-3-662-57546-8\n\n\n\n2018PhRvL.120b9901P\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nPustilnik, M.\nvan Heck, B.\nLutchyn, R. M.\nGlazman, L. I.\nPhysical Review Letters, Volume 120, Issue 2, id.029901\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nNot Available <P />\ndoi:10.1103/PhysRevLett.120.029901\n\n\n\n2017PhDT........14C\nResolving Gas-Phase Metallicity In Galaxies\nCarton, David\nPhD Thesis, Leiden University, 2017\n2017-06-01\ngalaxies: evolution, galaxies: abundances, galaxies: ISM\nhttps://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nChapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation. <P />Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies. <P />Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient. <P />Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas. <P />\ndoi:10.5281/zenodo.581221\n\n\n\n2017nova.pres.2388K\nA 3D View of a Supernova Remnant\nKohler, Susanna\nAAS Nova Highlight, 14 Jun 2017, id.2388\n2017-06-01\nFeatures, Highlights, interstellar medium, stellar evolution, supernova remnant, supernovae, white dwarfs\nhttps://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nThe outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384 <P />\n\n\n\n2017CBET.4403....2G\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\nGreen, D. W. E.\nCentral Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\n2017-06-01\nhttps://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nA previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg). <P />\n\n\n\n2017ascl.soft06009C\nsick: Spectroscopic inference crank\nCasey, Andrew R.\nAstrophysics Source Code Library, record ascl:1706.009\n2017-06-01\nSoftware\nhttps://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nsick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data. <P />\n\n\n\n2017yCat.113380453S\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nSiltala, J.\nJetsu, L.\nHackman, T.\nHenry, G. W.\nImmonen, L.\nKajatkari, P.\nLankinen, J.\nLehtinen, J.\nMonira, S.\nNikbakhsh, S.\nViitanen, A.\nViuho, J.\nWillamo, T.\nVizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\n2017-05-01\nStars: variable\nhttps://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nThe included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star. <P />The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />\n\n\n\n2017AAVSN.429....1W\nV694 Mon (MWC 560) spectroscopy requested\nWaagen, Elizabeth O.\nAAVSO Special Notice #429\n2017-05-01\nastronomical databases: miscellaneous, binaries: symbiotic, stars: individual (V694 Mon, MWC 560)\n(C) AAVSO 2017\nhttps://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nThe observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details. <P />\n\n\n\n2017sptz.prop13168Y\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nYan, Lin\nSpitzer Proposal ID 13168\n2017-04-01\nhttps://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event. <P />\n\n\n\n2017MsT..........2A\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAzankpo, Severin\nMasters thesis, University of Stellenbosch, March 2017, 120 pages\n2017-03-01\nhttps://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nThe African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads. <P />\n\n\n\n2016emo6.rept.....R\nThe penumbral Moon\'s eclipse form 16 september 2016\nRotaru, Adrian\nPteancu, Mircea\nZaharia, Cristian\nhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\n2016-10-01\nTHE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY\nhttps://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nThe web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon. <P />\n\n\n\n2016iac..talk..872V\nLiving on the edge: Adaptive Optics+Lucky Imaging\nVelasco, Sergio\nIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\n2016-03-01\nhttps://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nNot Available <P />\n\n\n\n2009bcet.book...65L\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\nLiu, Corey W.\nAlekseyev, Viktor Y.\nAllwardt, Jeffrey R.\nBankovich, Alexander J.\nCade-Menun, Barbara J.\nDavis, Ronald W.\nDu, Lin-Shu\nGarcia, K. Christopher\nHerschlag, Daniel\nKhosla, Chaitan\nKraut, Daniel A.\nLi, Qing\nNull, Brian\nPuglisi, Joseph D.\nSigala, Paul A.\nStebbins, Jonathan F.\nVarani, Luca\nBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\n2009-01-01\nPhysics\n(c) 2009: Springer Netherlands\nhttps://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nThe discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism. <P />\ndoi:10.1007/978-90-481-2368-1_5\n\n\n\n2007AAS...210.2104M\nTime Domain Exploration with the Palomar-QUEST Sky Survey\nMahabal, Ashish A.\nDrake, A. J.\nDjorgovski, S. G.\nDonalek, C.\nGlikman, E.\nGraham, M. J.\nWilliams, R.\nBaltay, C.\nRabinowitz, D.\nPQ Team Caltech\nYale\nNCSA\nIndiana\n, . . .\nAmerican Astronomical Society Meeting 210, id.21.04\n2007-05-01\nhttps://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nPalomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system. <P />Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys. <P />We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment. <P />The PQ survey is partially supported by the U.S. National Science Foundation (NSF). <P />\n\n\n\n2007RJPh....1...35.\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n., S. N. Agbo\n., E. C. Okoroigwe\nResearch Journal of Physics, vol. 1, issue 1, pp. 35-41\n2007-01-01\nhttps://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nNot Available <P />\ndoi:10.3923/rjp.2007.35.41\n\n\n\n1995ans..agar..390M\nSpacecraft navigation requirements\nMiller, Judy L.\nIn AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\n1995-06-01\nEarth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space Navigation, Spacecraft Trajectories, Support Systems, Technology Assessment, Technology Utilization, Ascent Trajectories, Reentry Trajectories, Spacecraft, Spacecraft Performance, Spacecraft Survivability, Tradeoffs, Weight (Mass), Space Communications, Spacecraft Communications, Command and Tracking\nhttps://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nSpacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy). <P />\n\n\n\n1995anda.book.....N\nApplied nonlinear dynamics: analytical, computational and experimental methods\nNayfeh, Ali H.\nBalachandran, Balakumar\nWiley series in nonlinear science, New York; Chichester: Wiley, |c1995\n1995-01-01\nhttps://ui.adsabs.harvard.edu/abs/1995anda.book.....N\ncitations:118\nNot Available <P />\n\n\n\n1991hep.th....8028G\nApplied Conformal Field Theory\nGinsparg, Paul\neprint arXiv:hep-th/9108028\n1988-11-01\nHigh Energy Physics - Theory\nhttps://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\ncitations:190\nThese lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications <P />\n\n\n\n1983aiaa.meetY....K\nAutonomous navigation using lunar beacons\nKhatib, A. R.\nEllis, J.\nFrench, J.\nNull, G.\nYunck, T.\nWu, S.\nAmerican Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\n1983-01-01\nArtificial Satellites, Autonomous Navigation, Earth-Moon System, Lunar Communication, Radio Beacons, Radio Navigation, Space Navigation, Doppler Navigation, Least Squares Method, Orbit Calculation, Space Communications, Spacecraft Communications, Command and Tracking\nhttps://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nThe concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation. <P />\n\n\n\n2012ddsw.rept.....T\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nThornton, P. E.\nThornton, M. M.\nMayer, B. W.\nWilhelmi, N.\nWei, Y.\nDevarakonda, R.\nCook, R.\nOak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\n2012-04-01\nDaymet\nOak Ridge National Laboratory\nhttps://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\ncitations:51\nArchived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\ndoi:10.3334/ORNLDAAC/1219\n\n\n\n2020EPJC...80...96D\nGeneralized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nDhaygude, Akanksha\nDesai, Shantanu\nThe European Physical Journal C, Volume 80, Issue 2, article id.96\n2020-02-01\nAstrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Nuclear Experiment\n© The Author(s) 2020\nhttps://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\nRecently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\ndoi:10.1140/epjc/s10052-020-7683-6; 10.48550/arXiv.1912.06970\n\n\n'} data_dublin_core_publisher = {'msg': 'Retrieved 5 abstracts, starting with number 1.', 'export': '\n\n\n2024zndo..10908474S\npc2/pqdts: v2024.2\nSchade, Robert\nZenodo\n2024-04-02\nhttps://ui.adsabs.harvard.edu/abs/2024zndo..10908474S\nChanges: improved installation mechanism for Julia spelling fixes in README.MD\ndoi:10.5281/zenodo.10908474\nZenodo\n\n\n\n2024wsp..conf...20V\nA modern view of former rivers on Mars.\nVidmachenko, A.\nProceedings of the VIII International Scientific and Practical Conference. World science priorities (February 08 – 09, 2024) Chapter Astronomy. Publisher: «World of Conferences». Vienna. Austria. P. 20-25. ISBN 978-92-44513-88-0.\n2024-02-01\nMars, riverbeds, meandering valleys, glaciers, eternal permafrost\nhttps://ui.adsabs.harvard.edu/abs/2024wsp..conf...20V\nNow the surface of Mars is a waterless desert, over which storms rage, raising sand and dust to a height of tens of kilometers. Under modern conditions, open bodies of water cannot exist on Mars. And water on the planet is contained either in the soil layer as permafrost, or in the form of open ice and snow; a very small amount of water is present in gaseous form in the atmosphere. The large reservoirs of water ice on Mars are the polar caps. Studies of Mars by spacecraft have shown that there is a huge amount of ice, and possibly liquid water, under the surface layer at a shallow depth. Analysis of the collected data allowed us to come to the conclusion that liquid water existed in significant quantities on the surface of Mars several billion years ago. That is, in the past, Mars had a full-fledged hydrosphere and a rather powerful atmosphere with a pressure near the surface of more than 0.4 bar. Later, the planet\'s climate changed. It lost much of its atmosphere and water, turning into a cold world. On the surface of Mars, there are numerous winding valleys with a long length, reminiscent of the dried-up channels of terrestrial rivers. A significant portion of the water that once flowed along currently dry riverbeds must now be under the surface of the planet. It is also possible that some channels are the result of the action of not liquid water, but a mixture of mud, ice and steam that flow only episodically. It is possible that the meandering valleys formed moving masses of glaciers. There is every reason to believe that there is still a lot of water on Mars, and it still exists in the form of permafrost. A perspective image of the Echus Chasma region suggests that liquid water was present on this part of the Martian surface up to a billion years ago. Later, the planet cooled down, the lakes froze, and glaciers formed, which \'cut\' the Kasei Valles with their streams.\nWorld of Conferences\n\n\n\n2024asal.book..204V\nNew generation telescopes for the astronomy of the future.\nVidmachenko, A.\nIn book: Astronomical almanac, 70, Edition: MAO NAS of Ukraine. Publisher: Kyiv, Akademperiodika, p. 204-209.\n2024-01-01\nnew astronomical instruments, Telescopes, telescope construction, astronomical research\nhttps://ui.adsabs.harvard.edu/abs/2024asal.book..204V\nIn the next few years, several new astronomical instruments are planned to be launched on Earth and in space. Each of these devices is very expensive! But many countries allocate large amounts of money for this, and plan to receive more and more recent data about the surrounding universe. Telescopes are devices for observing distant objects. The very first working telescope was created in 1608 by the Dutch optician Hans Lippersgei. The creation of the telescope was also attributed to such masters as another Dutch eyeglass maker from Middelburg, Zachary Janssen, and Jacob Mathews from the city of Alkmaar. These earliest telescopes consisted of a convex lens as an objective and a concave lens that served as an eyepiece. In 1609, Galileo Galilei significantly improved the design of the telescope, achieving a 30-fold increase in the original images. With its help, Galileo performed the first survey of the heavenly bodies. Therefore, even now, the creation of astronomical instruments, whose characteristics significantly improve previous examples of telescope construction, is considered extremely important in astronomical research. The Hubble telescope was the first to provide interesting information about the features of images of the most distant galaxies. They are significantly different from those formed relatively recently. One of the world\'s largest ground-based telescopes, the Giant Magellan Telescope, is under construction. It is being built in Chile and its gradual commissioning will begin in 2024. Segments of seven monolithic mirrors, with a diameter of 8.4 m each, create an optical surface with an equivalent diameter of 24.5 m. Larger will be the 30-meter telescope, which is planned to be built on the island of Hawaii, next to the two 9-meter Keck reflectors at the Mauna Kea observatory. The mirror surface of this telescope will consist of almost five hundred hexagonal segments and will reach a diameter of 30 m. It is expected to be tested in 2027. In 2014, the European Southern Observatory started the construction of the Extremely Large Telescope. In 2025, it is planned to become the most powerful optical astronomical instrument in the world, with an equivalent diameter of its mirror surface of 39 m.\nKyiv\n\n\n\n2018scrp.conf.....K\nScience and Computing with Raspberry Pi\nKent, Brian R.\nScience and Computing with Raspberry Pi, by Brian R. Kent. Online ISBN: 978-1-6817-4996-9, Print ISBN: 978-1-6817-4993-8, Morgan &amp; Claypool Publishers, 2018\n2018-07-01\nsingle board computing, astronomy, very large array, astrophysics, visualization, data science, computing, radio astronomy\nCopyright (c) 2018 Morgan & Claypool Publishers\nhttps://ui.adsabs.harvard.edu/abs/2018scrp.conf.....K\nThe portable Raspberry Pi computing platform with the power of Linux yields an exciting exploratory tool for beginning scientific computing. Science and Computing with Raspberry Pi takes the reader through explorations in a variety of computing exercises with the physical sciences. The book guides the user through: configuring your Raspberry Pi and Linux operating system; understanding the software requirements while using the Pi for scientific computing; computing exercises in physics, astronomy, chaos theory, and machine learning.\nMorgan & Claypool\n\n\n\n2023uwff.book.....R\nUnder the weather: a future forecast for New Zealand\nRenwick, J. A.\nUnder the weather: a future forecast for New Zealand, by J. A. Renwick, 2023. Auckland: HarperCollins Publishers. OCLC: 1388369161. ISBN: 9781775541721.\n2023-01-01\nhttps://ui.adsabs.harvard.edu/abs/2023uwff.book.....R\nA forecast for New Zealand\'s changing climate and why it matters to our everyday lives A warmer world will change more than just our weather patterns. It will change the look of the land around us, what grows and lives on it - including us. Drawing on climate models that can travel to ice ages and hothouses of the deep past, Professor James Renwick untangles how we know exactly what the future holds and why it matters to our everyday lives. He looks at New Zealand\'s more frequent natural disasters, warming and increasingly acidic waters, the creep of rising sea levels, and the ways that the changing weather will affect our agriculture, lifestyle, food security and economy.Arresting, galvanizing and clear-sighted, Under the Weather is a picture of a miraculous planet in danger, a stock-take on what it means for this small country, and a reminder that the shape of our future is up to us.\'--Publisher description.\nHarperCollins\n\n\n'} -data_ref = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '\n\n\n2018Wthr...73Q..35.\nBook reviews\nWeather, vol. 73, issue 1, pp. 35-35\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Wthr...73Q..35./abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Wthr...73Q..35./PUB_HTML\n\n10.1002/wea.3072\n\n\n\n2018TDM.....5a0201F\n2D Materials: maintaining editorial quality\nFal\'ko, Vladimir\nThomas, Ceri-Wyn\n2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018TDM.....5a0201F/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018TDM.....5a0201F/PUB_HTML\n\n10.1088/2053-1583/aa9403\n\n\n\n2018Spin....877001P\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nParkin, Stuart\nChantrell, Roy\nChang, Ching-Ray\nSpin, Volume 8, Issue 4, id. 1877001\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/PUB_HTML\n\n\nPublisher PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/PUB_PDF\n\n10.1142/S2010324718770015\n\n\n\n2018SAAS...38.....D\nMillimeter Astronomy\nDessauges-Zavadsky, Miroslava\nPfenniger, Daniel\nMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/coreads\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/toc\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/PUB_HTML\n\n10.1007/978-3-662-57546-8\n\n\n\n2018PhRvL.120b9901P\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nPustilnik, M.\nvan Heck, B.\nLutchyn, R. M.\nGlazman, L. I.\nPhysical Review Letters, Volume 120, Issue 2, id.029901\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/reference\n4\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/PUB_HTML\n\n10.1103/PhysRevLett.120.029901\n\n\n\n2017PhDT........14C\nResolving Gas-Phase Metallicity In Galaxies\nCarton, David\nPhD Thesis, Leiden University, 2017\nJun 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/reference\n1\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/PUB_HTML\n\n10.5281/zenodo.581221\n\n\n\n2017nova.pres.2388K\nA 3D View of a Supernova Remnant\nKohler, Susanna\nAAS Nova Highlight, 14 Jun 2017, id.2388\nJun 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/PUB_HTML\n\n\nChandra X-Ray Observatory\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/Chandra\n1\n\n\n\n\n2017CBET.4403....2G\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\nGreen, D. W. E.\nCentral Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\nJun 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017CBET.4403....2G/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017CBET.4403....2G/PUB_HTML\n\n\n\n\n2017ascl.soft06009C\nsick: Spectroscopic inference crank\nCasey, Andrew R.\nAstrophysics Source Code Library, record ascl:1706.009\nJun 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017ascl.soft06009C/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017ascl.soft06009C/PUB_HTML\n\nascl:1706.009\n\n\n\n2017yCat.113380453S\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nSiltala, J.\nJetsu, L.\nHackman, T.\nHenry, G. W.\nImmonen, L.\nKajatkari, P.\nLankinen, J.\nLehtinen, J.\nMonira, S.\nNikbakhsh, S.\nViitanen, A.\nViuho, J.\nWillamo, T.\nVizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\nMay 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017yCat.113380453S/abstract\n\n\nVizieR Catalog Service\nhttps://ui.adsabs.harvard.edu/link_gateway/2017yCat.113380453S/Vizier\n1\n\n\n\n\n2017AAVSN.429....1W\nV694 Mon (MWC 560) spectroscopy requested\nWaagen, Elizabeth O.\nAAVSO Special Notice #429\nMay 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/reference\n6\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/PUB_HTML\n\n\n\n\n2017sptz.prop13168Y\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nYan, Lin\nSpitzer Proposal ID 13168\nApr 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017sptz.prop13168Y/abstract\n\n\nSpitzer Space Telescope\nhttps://ui.adsabs.harvard.edu/link_gateway/2017sptz.prop13168Y/Spitzer\n1\n\n\n\n\n2017MsT..........2A\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAzankpo, Severin\nMasters thesis, University of Stellenbosch, March 2017, 120 pages\nMar 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/reference\n4\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/PUB_HTML\n\n\nAuthor PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/AUTHOR_PDF\n\n\nPublisher PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/PUB_PDF\n\n\n\n\n2016emo6.rept.....R\nThe penumbral Moon\'s eclipse form 16 september 2016\nRotaru, Adrian\nPteancu, Mircea\nZaharia, Cristian\nhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\nOct 2016\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2016emo6.rept.....R/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2016emo6.rept.....R/coreads\n\n\n\n\n2016iac..talk..872V\nLiving on the edge: Adaptive Optics+Lucky Imaging\nVelasco, Sergio\nIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\nMar 2016\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/reference\n1\n\n\nAuthor Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/AUTHOR_HTML\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/PUB_HTML\n\n\n\n\n2009bcet.book...65L\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\nLiu, Corey W.\nAlekseyev, Viktor Y.\nAllwardt, Jeffrey R.\nBankovich, Alexander J.\nCade-Menun, Barbara J.\nDavis, Ronald W.\nDu, Lin-Shu\nGarcia, K. Christopher\nHerschlag, Daniel\nKhosla, Chaitan\nKraut, Daniel A.\nLi, Qing\nNull, Brian\nPuglisi, Joseph D.\nSigala, Paul A.\nStebbins, Jonathan F.\nVarani, Luca\nBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\nJan 2009\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/abstract\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/toc\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/PUB_HTML\n\n10.1007/978-90-481-2368-1_5\n\n\n\n2007AAS...210.2104M\nTime Domain Exploration with the Palomar-QUEST Sky Survey\nMahabal, Ashish A.\nDrake, A. J.\nDjorgovski, S. G.\nDonalek, C.\nGlikman, E.\nGraham, M. J.\nWilliams, R.\nBaltay, C.\nRabinowitz, D.\nPQ Team Caltech\nYale\nNCSA\nIndiana\n, . . .\nAmerican Astronomical Society Meeting 210, id.21.04\nMay 2007\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2007AAS...210.2104M/abstract\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2007AAS...210.2104M/toc\n\n\n\n\n2007RJPh....1...35.\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n., S. N. Agbo\n., E. C. Okoroigwe\nResearch Journal of Physics, vol. 1, issue 1, pp. 35-41\nJan 2007\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2007RJPh....1...35./abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2007RJPh....1...35./PUB_HTML\n\n10.3923/rjp.2007.35.41\n\n\n\n1995ans..agar..390M\nSpacecraft navigation requirements\nMiller, Judy L.\nIn AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\nJun 1995\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1995ans..agar..390M/abstract\n\n\n\n\n1995anda.book.....N\nApplied nonlinear dynamics: analytical, computational and experimental methods\nNayfeh, Ali H.\nBalachandran, Balakumar\nWiley series in nonlinear science, New York; Chichester: Wiley, |c1995\nJan 1995\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/citations\n118\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/coreads\n\n118\n\n\n\n1991hep.th....8028G\nApplied Conformal Field Theory\nGinsparg, Paul\neprint arXiv:hep-th/9108028\nNov 1988\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/citations\n190\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/coreads\n\n\narXiv Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/EPRINT_HTML\n\n\narXiv PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/EPRINT_PDF\n\n190\narXiv:hep-th/9108028\n\n\n\n1983aiaa.meetY....K\nAutonomous navigation using lunar beacons\nKhatib, A. R.\nEllis, J.\nFrench, J.\nNull, G.\nYunck, T.\nWu, S.\nAmerican Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\nJan 1983\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1983aiaa.meetY....K/abstract\n\n\n\n\n2012ddsw.rept.....T\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nThornton, P. E.\nThornton, M. M.\nMayer, B. W.\nWilhelmi, N.\nWei, Y.\nDevarakonda, R.\nCook, R.\nOak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\nApr 2012\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/citations\n51\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/PUB_HTML\n\n51\n10.3334/ORNLDAAC/1219\n\n\n'} +data_ref = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '\n\n\n2018Wthr...73Q..35.\nBook reviews\nWeather, vol. 73, issue 1, pp. 35-35\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Wthr...73Q..35./abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Wthr...73Q..35./PUB_HTML\n\n10.1002/wea.3072\n\n\n\n2018TDM.....5a0201F\n2D Materials: maintaining editorial quality\nFal\'ko, Vladimir\nThomas, Ceri-Wyn\n2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018TDM.....5a0201F/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018TDM.....5a0201F/PUB_HTML\n\n10.1088/2053-1583/aa9403\n\n\n\n2018Spin....877001P\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nParkin, Stuart\nChantrell, Roy\nChang, Ching-Ray\nSpin, Volume 8, Issue 4, id. 1877001\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/PUB_HTML\n\n\nPublisher PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/PUB_PDF\n\n10.1142/S2010324718770015\n\n\n\n2018SAAS...38.....D\nMillimeter Astronomy\nDessauges-Zavadsky, Miroslava\nPfenniger, Daniel\nMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/coreads\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/toc\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/PUB_HTML\n\n10.1007/978-3-662-57546-8\n\n\n\n2018PhRvL.120b9901P\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nPustilnik, M.\nvan Heck, B.\nLutchyn, R. M.\nGlazman, L. I.\nPhysical Review Letters, Volume 120, Issue 2, id.029901\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/reference\n4\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/PUB_HTML\n\n10.1103/PhysRevLett.120.029901\n\n\n\n2017PhDT........14C\nResolving Gas-Phase Metallicity In Galaxies\nCarton, David\nPhD Thesis, Leiden University, 2017\nJun 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/reference\n1\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/PUB_HTML\n\n10.5281/zenodo.581221\n\n\n\n2017nova.pres.2388K\nA 3D View of a Supernova Remnant\nKohler, Susanna\nAAS Nova Highlight, 14 Jun 2017, id.2388\nJun 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/PUB_HTML\n\n\nChandra X-Ray Observatory\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/Chandra\n1\n\n\n\n\n2017CBET.4403....2G\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\nGreen, D. W. E.\nCentral Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\nJun 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017CBET.4403....2G/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017CBET.4403....2G/PUB_HTML\n\n\n\n\n2017ascl.soft06009C\nsick: Spectroscopic inference crank\nCasey, Andrew R.\nAstrophysics Source Code Library, record ascl:1706.009\nJun 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017ascl.soft06009C/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017ascl.soft06009C/PUB_HTML\n\nascl:1706.009\n\n\n\n2017yCat.113380453S\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nSiltala, J.\nJetsu, L.\nHackman, T.\nHenry, G. W.\nImmonen, L.\nKajatkari, P.\nLankinen, J.\nLehtinen, J.\nMonira, S.\nNikbakhsh, S.\nViitanen, A.\nViuho, J.\nWillamo, T.\nVizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\nMay 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017yCat.113380453S/abstract\n\n\nVizieR Catalog Service\nhttps://ui.adsabs.harvard.edu/link_gateway/2017yCat.113380453S/Vizier\n1\n\n\n\n\n2017AAVSN.429....1W\nV694 Mon (MWC 560) spectroscopy requested\nWaagen, Elizabeth O.\nAAVSO Special Notice #429\nMay 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/reference\n6\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/PUB_HTML\n\n\n\n\n2017sptz.prop13168Y\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nYan, Lin\nSpitzer Proposal ID 13168\nApr 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017sptz.prop13168Y/abstract\n\n\nSpitzer Space Telescope\nhttps://ui.adsabs.harvard.edu/link_gateway/2017sptz.prop13168Y/Spitzer\n1\n\n\n\n\n2017MsT..........2A\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAzankpo, Severin\nMasters thesis, University of Stellenbosch, March 2017, 120 pages\nMar 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/reference\n4\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/PUB_HTML\n\n\nAuthor PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/AUTHOR_PDF\n\n\nPublisher PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/PUB_PDF\n\n\n\n\n2016emo6.rept.....R\nThe penumbral Moon\'s eclipse form 16 september 2016\nRotaru, Adrian\nPteancu, Mircea\nZaharia, Cristian\nhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\nOct 2016\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2016emo6.rept.....R/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2016emo6.rept.....R/coreads\n\n\n\n\n2016iac..talk..872V\nLiving on the edge: Adaptive Optics+Lucky Imaging\nVelasco, Sergio\nIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\nMar 2016\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/reference\n1\n\n\nAuthor Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/AUTHOR_HTML\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/PUB_HTML\n\n\n\n\n2009bcet.book...65L\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\nLiu, Corey W.\nAlekseyev, Viktor Y.\nAllwardt, Jeffrey R.\nBankovich, Alexander J.\nCade-Menun, Barbara J.\nDavis, Ronald W.\nDu, Lin-Shu\nGarcia, K. Christopher\nHerschlag, Daniel\nKhosla, Chaitan\nKraut, Daniel A.\nLi, Qing\nNull, Brian\nPuglisi, Joseph D.\nSigala, Paul A.\nStebbins, Jonathan F.\nVarani, Luca\nBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\nJan 2009\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/abstract\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/toc\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/PUB_HTML\n\n10.1007/978-90-481-2368-1_5\n\n\n\n2007AAS...210.2104M\nTime Domain Exploration with the Palomar-QUEST Sky Survey\nMahabal, Ashish A.\nDrake, A. J.\nDjorgovski, S. G.\nDonalek, C.\nGlikman, E.\nGraham, M. J.\nWilliams, R.\nBaltay, C.\nRabinowitz, D.\nPQ Team Caltech\nYale\nNCSA\nIndiana\n, . . .\nAmerican Astronomical Society Meeting 210, id.21.04\nMay 2007\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2007AAS...210.2104M/abstract\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2007AAS...210.2104M/toc\n\n\n\n\n2007RJPh....1...35.\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n., S. N. Agbo\n., E. C. Okoroigwe\nResearch Journal of Physics, vol. 1, issue 1, pp. 35-41\nJan 2007\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2007RJPh....1...35./abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2007RJPh....1...35./PUB_HTML\n\n10.3923/rjp.2007.35.41\n\n\n\n1995ans..agar..390M\nSpacecraft navigation requirements\nMiller, Judy L.\nIn AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\nJun 1995\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1995ans..agar..390M/abstract\n\n\n\n\n1995anda.book.....N\nApplied nonlinear dynamics: analytical, computational and experimental methods\nNayfeh, Ali H.\nBalachandran, Balakumar\nWiley series in nonlinear science, New York; Chichester: Wiley, |c1995\nJan 1995\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/citations\n118\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/coreads\n\n118\n\n\n\n1991hep.th....8028G\nApplied Conformal Field Theory\nGinsparg, Paul\neprint arXiv:hep-th/9108028\nNov 1988\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/citations\n190\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/coreads\n\n\narXiv Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/EPRINT_HTML\n\n\narXiv PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/EPRINT_PDF\n\n190\narXiv:hep-th/9108028\n\n\n\n1983aiaa.meetY....K\nAutonomous navigation using lunar beacons\nKhatib, A. R.\nEllis, J.\nFrench, J.\nNull, G.\nYunck, T.\nWu, S.\nAmerican Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\nJan 1983\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1983aiaa.meetY....K/abstract\n\n\n\n\n2012ddsw.rept.....T\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nThornton, P. E.\nThornton, M. M.\nMayer, B. W.\nWilhelmi, N.\nWei, Y.\nDevarakonda, R.\nCook, R.\nOak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\nApr 2012\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/citations\n51\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/PUB_HTML\n\n51\n10.3334/ORNLDAAC/1219\n\n\n\n2020EPJC...80...96D\nGeneralized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nDhaygude, Akanksha\nDesai, Shantanu\nThe European Physical Journal C, Volume 80, Issue 2, article id.96\nFeb 2020\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/coreads\n\n\narXiv Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/EPRINT_HTML\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/PUB_HTML\n\n\narXiv PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/EPRINT_PDF\n\n10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\narXiv:1912.06970\n\n\n'} -data_ref_with_abs = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '\n\n\n2018Wthr...73Q..35.\nBook reviews\nWeather, vol. 73, issue 1, pp. 35-35\n73\nJan 2018\n35\n35\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Wthr...73Q..35./abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Wthr...73Q..35./PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nNot Available <P />\n10.1002/wea.3072\n\n\n\n2018TDM.....5a0201F\n2D Materials: maintaining editorial quality\nFal\'ko, Vladimir\nThomas, Ceri-Wyn\nAA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\n2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\n5\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018TDM.....5a0201F/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018TDM.....5a0201F/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nNot Available <P />\n10.1088/2053-1583/aa9403\n\n\n\n2018Spin....877001P\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nParkin, Stuart\nChantrell, Roy\nChang, Ching-Ray\nSpin, Volume 8, Issue 4, id. 1877001\n8\nJan 2018\n(c) 2018: World Scientific Publishing Company\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/PUB_HTML\n\n\nPublisher PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/PUB_PDF\n\nhttps://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nNot Available <P />\n10.1142/S2010324718770015\n\n\n\n2018SAAS...38.....D\nMillimeter Astronomy\nDessauges-Zavadsky, Miroslava\nPfenniger, Daniel\nMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\n38\nJan 2018\n\nPhysics\n\n(c) 2018: Springer-Verlag GmbH Germany, part of Springer Nature\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/coreads\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/toc\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nNot Available <P />\n10.1007/978-3-662-57546-8\n\n\n\n2018PhRvL.120b9901P\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nPustilnik, M.\nvan Heck, B.\nLutchyn, R. M.\nGlazman, L. I.\nPhysical Review Letters, Volume 120, Issue 2, id.029901\n120\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/reference\n4\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nNot Available <P />\n10.1103/PhysRevLett.120.029901\n\n\n\n2017PhDT........14C\nResolving Gas-Phase Metallicity In Galaxies\nCarton, David\nAA(Leiden University)\nPhD Thesis, Leiden University, 2017\nJun 2017\n\ngalaxies: evolution\ngalaxies: abundances\ngalaxies: ISM\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/reference\n1\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nChapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation. <P />Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies. <P />Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient. <P />Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas. <P />\n10.5281/zenodo.581221\n\n\n\n2017nova.pres.2388K\nA 3D View of a Supernova Remnant\nKohler, Susanna\nAAS Nova Highlight, 14 Jun 2017, id.2388\nJun 2017\n\nFeatures\nHighlights\ninterstellar medium\nstellar evolution\nsupernova remnant\nsupernovae\nwhite dwarfs\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/PUB_HTML\n\n\nChandra X-Ray Observatory\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/Chandra\n1\n\nhttps://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nThe outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384 <P />\n\n\n\n2017CBET.4403....2G\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\nGreen, D. W. E.\nCentral Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\n4403\nJun 2017\n2\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017CBET.4403....2G/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017CBET.4403....2G/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nA previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg). <P />\n\n\n\n2017ascl.soft06009C\nsick: Spectroscopic inference crank\nCasey, Andrew R.\nAstrophysics Source Code Library, record ascl:1706.009\nJun 2017\n\nSoftware\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017ascl.soft06009C/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017ascl.soft06009C/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nsick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data. <P />\nascl:1706.009\n\n\n\n2017yCat.113380453S\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nSiltala, J.\nJetsu, L.\nHackman, T.\nHenry, G. W.\nImmonen, L.\nKajatkari, P.\nLankinen, J.\nLehtinen, J.\nMonira, S.\nNikbakhsh, S.\nViitanen, A.\nViuho, J.\nWillamo, T.\nVizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\nMay 2017\n\nStars: variable\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017yCat.113380453S/abstract\n\n\nVizieR Catalog Service\nhttps://ui.adsabs.harvard.edu/link_gateway/2017yCat.113380453S/Vizier\n1\n\nhttps://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nThe included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star. <P />The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />\n\n\n\n2017AAVSN.429....1W\nV694 Mon (MWC 560) spectroscopy requested\nWaagen, Elizabeth O.\nAA(AAVSO)\nAAVSO Special Notice #429\n429\nMay 2017\n1\n\nastronomical databases: miscellaneous\nbinaries: symbiotic\nstars: individual (V694 Mon\nMWC 560)\n\n(C) AAVSO 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/reference\n6\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nThe observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details. <P />\n\n\n\n2017sptz.prop13168Y\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nYan, Lin\nSpitzer Proposal ID 13168\nApr 2017\n13168\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017sptz.prop13168Y/abstract\n\n\nSpitzer Space Telescope\nhttps://ui.adsabs.harvard.edu/link_gateway/2017sptz.prop13168Y/Spitzer\n1\n\nhttps://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event. <P />\n\n\n\n2017MsT..........2A\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAzankpo, Severin\nAA(University of Stellenbosch)\nMasters thesis, University of Stellenbosch, March 2017, 120 pages\nMar 2017\n2\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/reference\n4\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/PUB_HTML\n\n\nAuthor PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/AUTHOR_PDF\n\n\nPublisher PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/PUB_PDF\n\nhttps://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nThe African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads. <P />\n\n\n\n2016emo6.rept.....R\nThe penumbral Moon\'s eclipse form 16 september 2016\nRotaru, Adrian\nPteancu, Mircea\nZaharia, Cristian\nAA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\nOct 2016\n\nTHE MOON\nECLIPSES\nPARTIAL\nPENUMBRAL\nASTROPHOTOGRAPHY\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2016emo6.rept.....R/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2016emo6.rept.....R/coreads\n\nhttps://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nThe web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon. <P />\n\n\n\n2016iac..talk..872V\nLiving on the edge: Adaptive Optics+Lucky Imaging\nVelasco, Sergio\nAA(Instituto de Astrofísica de Canarias)\nIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\nMar 2016\n872\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/reference\n1\n\n\nAuthor Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/AUTHOR_HTML\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nNot Available <P />\n\n\n\n2009bcet.book...65L\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\nLiu, Corey W.\nAlekseyev, Viktor Y.\nAllwardt, Jeffrey R.\nBankovich, Alexander J.\nCade-Menun, Barbara J.\nDavis, Ronald W.\nDu, Lin-Shu\nGarcia, K. Christopher\nHerschlag, Daniel\nKhosla, Chaitan\nKraut, Daniel A.\nLi, Qing\nNull, Brian\nPuglisi, Joseph D.\nSigala, Paul A.\nStebbins, Jonathan F.\nVarani, Luca\nAA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological &amp; Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological &amp; Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological &amp; Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological &amp; Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\nJan 2009\n65\n\nPhysics\n\n(c) 2009: Springer Netherlands\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/abstract\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/toc\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nThe discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism. <P />\n10.1007/978-90-481-2368-1_5\n\n\n\n2007AAS...210.2104M\nTime Domain Exploration with the Palomar-QUEST Sky Survey\nMahabal, Ashish A.\nDrake, A. J.\nDjorgovski, S. G.\nDonalek, C.\nGlikman, E.\nGraham, M. J.\nWilliams, R.\nBaltay, C.\nRabinowitz, D.\nPQ Team Caltech\nYale\nNCSA\nIndiana\n, . . .\nAA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nAmerican Astronomical Society Meeting 210, id.21.04\n210\nMay 2007\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2007AAS...210.2104M/abstract\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2007AAS...210.2104M/toc\n\nhttps://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nPalomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system. <P />Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys. <P />We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment. <P />The PQ survey is partially supported by the U.S. National Science Foundation (NSF). <P />\n\n\n\n2007RJPh....1...35.\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n., S. N. Agbo\n., E. C. Okoroigwe\nResearch Journal of Physics, vol. 1, issue 1, pp. 35-41\n1\nJan 2007\n35\n41\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2007RJPh....1...35./abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2007RJPh....1...35./PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nNot Available <P />\n10.3923/rjp.2007.35.41\n\n\n\n1995ans..agar..390M\nSpacecraft navigation requirements\nMiller, Judy L.\nAA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nIn AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\nJun 1995\n390\n405\n\nEarth Orbits\nNavigation Aids\nNavigators\nOnboard Equipment\nSpace Navigation\nSpacecraft Trajectories\nSupport Systems\nTechnology Assessment\nTechnology Utilization\nAscent Trajectories\nReentry Trajectories\nSpacecraft\nSpacecraft Performance\nSpacecraft Survivability\nTradeoffs\nWeight (Mass)\nSpace Communications, Spacecraft Communications, Command and Tracking\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1995ans..agar..390M/abstract\n\nhttps://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nSpacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy). <P />\n\n\n\n1995anda.book.....N\nApplied nonlinear dynamics: analytical, computational and experimental methods\nNayfeh, Ali H.\nBalachandran, Balakumar\nWiley series in nonlinear science, New York; Chichester: Wiley, |c1995\nJan 1995\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/citations\n118\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/coreads\n\nhttps://ui.adsabs.harvard.edu/abs/1995anda.book.....N\n118\nNot Available <P />\n\n\n\n1991hep.th....8028G\nApplied Conformal Field Theory\nGinsparg, Paul\neprint arXiv:hep-th/9108028\nNov 1988\n\nHigh Energy Physics - Theory\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/citations\n190\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/coreads\n\n\narXiv Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/EPRINT_HTML\n\n\narXiv PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/EPRINT_PDF\n\nhttps://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\n190\nThese lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications <P />\narXiv:hep-th/9108028\n\n\n\n1983aiaa.meetY....K\nAutonomous navigation using lunar beacons\nKhatib, A. R.\nEllis, J.\nFrench, J.\nNull, G.\nYunck, T.\nWu, S.\nAA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nAmerican Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\nJan 1983\n\nArtificial Satellites\nAutonomous Navigation\nEarth-Moon System\nLunar Communication\nRadio Beacons\nRadio Navigation\nSpace Navigation\nDoppler Navigation\nLeast Squares Method\nOrbit Calculation\nSpace Communications, Spacecraft Communications, Command and Tracking\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1983aiaa.meetY....K/abstract\n\nhttps://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nThe concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation. <P />\n\n\n\n2012ddsw.rept.....T\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nThornton, P. E.\nThornton, M. M.\nMayer, B. W.\nWilhelmi, N.\nWei, Y.\nDevarakonda, R.\nCook, R.\nOak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\nApr 2012\n\nDaymet\n\nOak Ridge National Laboratory\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/citations\n51\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\n51\nArchived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\n10.3334/ORNLDAAC/1219\n\n\n'} +data_ref_with_abs = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '\n\n\n2018Wthr...73Q..35.\nBook reviews\nWeather, vol. 73, issue 1, pp. 35-35\n73\nJan 2018\n35\n35\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Wthr...73Q..35./abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Wthr...73Q..35./PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nNot Available <P />\n10.1002/wea.3072\n\n\n\n2018TDM.....5a0201F\n2D Materials: maintaining editorial quality\nFal\'ko, Vladimir\nThomas, Ceri-Wyn\nAA(Editor in Chief, National Graphene Institute, University of Manchester, United Kingdom), AB(Publisher, IOP Publishing, Bristol, United Kingdom)\n2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\n5\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018TDM.....5a0201F/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018TDM.....5a0201F/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nNot Available <P />\n10.1088/2053-1583/aa9403\n\n\n\n2018Spin....877001P\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nParkin, Stuart\nChantrell, Roy\nChang, Ching-Ray\nSpin, Volume 8, Issue 4, id. 1877001\n8\nJan 2018\n(c) 2018: World Scientific Publishing Company\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/PUB_HTML\n\n\nPublisher PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2018Spin....877001P/PUB_PDF\n\nhttps://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nNot Available <P />\n10.1142/S2010324718770015\n\n\n\n2018SAAS...38.....D\nMillimeter Astronomy\nDessauges-Zavadsky, Miroslava\nPfenniger, Daniel\nMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\n38\nJan 2018\n\nPhysics\n\n(c) 2018: Springer-Verlag GmbH Germany, part of Springer Nature\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/coreads\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/toc\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018SAAS...38.....D/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nNot Available <P />\n10.1007/978-3-662-57546-8\n\n\n\n2018PhRvL.120b9901P\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nPustilnik, M.\nvan Heck, B.\nLutchyn, R. M.\nGlazman, L. I.\nPhysical Review Letters, Volume 120, Issue 2, id.029901\n120\nJan 2018\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/reference\n4\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018PhRvL.120b9901P/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nNot Available <P />\n10.1103/PhysRevLett.120.029901\n\n\n\n2017PhDT........14C\nResolving Gas-Phase Metallicity In Galaxies\nCarton, David\nAA(Leiden University)\nPhD Thesis, Leiden University, 2017\nJun 2017\n\ngalaxies: evolution\ngalaxies: abundances\ngalaxies: ISM\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/reference\n1\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017PhDT........14C/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nChapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation. <P />Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies. <P />Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient. <P />Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas. <P />\n10.5281/zenodo.581221\n\n\n\n2017nova.pres.2388K\nA 3D View of a Supernova Remnant\nKohler, Susanna\nAAS Nova Highlight, 14 Jun 2017, id.2388\nJun 2017\n\nFeatures\nHighlights\ninterstellar medium\nstellar evolution\nsupernova remnant\nsupernovae\nwhite dwarfs\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/PUB_HTML\n\n\nChandra X-Ray Observatory\nhttps://ui.adsabs.harvard.edu/link_gateway/2017nova.pres.2388K/Chandra\n1\n\nhttps://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nThe outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384 <P />\n\n\n\n2017CBET.4403....2G\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\nGreen, D. W. E.\nCentral Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\n4403\nJun 2017\n2\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017CBET.4403....2G/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017CBET.4403....2G/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nA previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg). <P />\n\n\n\n2017ascl.soft06009C\nsick: Spectroscopic inference crank\nCasey, Andrew R.\nAstrophysics Source Code Library, record ascl:1706.009\nJun 2017\n\nSoftware\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017ascl.soft06009C/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017ascl.soft06009C/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nsick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data. <P />\nascl:1706.009\n\n\n\n2017yCat.113380453S\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nSiltala, J.\nJetsu, L.\nHackman, T.\nHenry, G. W.\nImmonen, L.\nKajatkari, P.\nLankinen, J.\nLehtinen, J.\nMonira, S.\nNikbakhsh, S.\nViitanen, A.\nViuho, J.\nWillamo, T.\nVizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\nMay 2017\n\nStars: variable\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017yCat.113380453S/abstract\n\n\nVizieR Catalog Service\nhttps://ui.adsabs.harvard.edu/link_gateway/2017yCat.113380453S/Vizier\n1\n\nhttps://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nThe included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star. <P />The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />\n\n\n\n2017AAVSN.429....1W\nV694 Mon (MWC 560) spectroscopy requested\nWaagen, Elizabeth O.\nAA(AAVSO)\nAAVSO Special Notice #429\n429\nMay 2017\n1\n\nastronomical databases: miscellaneous\nbinaries: symbiotic\nstars: individual (V694 Mon\nMWC 560)\n\n(C) AAVSO 2017\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/reference\n6\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017AAVSN.429....1W/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nThe observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details. <P />\n\n\n\n2017sptz.prop13168Y\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nYan, Lin\nSpitzer Proposal ID 13168\nApr 2017\n13168\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017sptz.prop13168Y/abstract\n\n\nSpitzer Space Telescope\nhttps://ui.adsabs.harvard.edu/link_gateway/2017sptz.prop13168Y/Spitzer\n1\n\nhttps://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event. <P />\n\n\n\n2017MsT..........2A\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAzankpo, Severin\nAA(University of Stellenbosch)\nMasters thesis, University of Stellenbosch, March 2017, 120 pages\nMar 2017\n2\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/reference\n4\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/PUB_HTML\n\n\nAuthor PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/AUTHOR_PDF\n\n\nPublisher PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2017MsT..........2A/PUB_PDF\n\nhttps://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nThe African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads. <P />\n\n\n\n2016emo6.rept.....R\nThe penumbral Moon\'s eclipse form 16 september 2016\nRotaru, Adrian\nPteancu, Mircea\nZaharia, Cristian\nAA(Bragadiru, Romania), AB(Private Astronomical Observatory, Arad, Romania), AC(Private Astronomical Observatory, Ploiesti, Romania)\nhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\nOct 2016\n\nTHE MOON\nECLIPSES\nPARTIAL\nPENUMBRAL\nASTROPHOTOGRAPHY\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2016emo6.rept.....R/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2016emo6.rept.....R/coreads\n\nhttps://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nThe web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon. <P />\n\n\n\n2016iac..talk..872V\nLiving on the edge: Adaptive Optics+Lucky Imaging\nVelasco, Sergio\nAA(Instituto de Astrofísica de Canarias)\nIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\nMar 2016\n872\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/abstract\n\n\nReferences in the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/reference\n1\n\n\nAuthor Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/AUTHOR_HTML\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2016iac..talk..872V/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nNot Available <P />\n\n\n\n2009bcet.book...65L\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\nLiu, Corey W.\nAlekseyev, Viktor Y.\nAllwardt, Jeffrey R.\nBankovich, Alexander J.\nCade-Menun, Barbara J.\nDavis, Ronald W.\nDu, Lin-Shu\nGarcia, K. Christopher\nHerschlag, Daniel\nKhosla, Chaitan\nKraut, Daniel A.\nLi, Qing\nNull, Brian\nPuglisi, Joseph D.\nSigala, Paul A.\nStebbins, Jonathan F.\nVarani, Luca\nAA(Stanford Magnetic Resonance Laboratory, Stanford University), AB(Department of Chemistry, Stanford University; , Genencor), AC(Department of Geological &amp; Environmental Sciences, Stanford University; , ConocoPhillips Company), AD(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AE(Department of Geological &amp; Environmental Sciences, Stanford University; , Agriculture and Agri-Food Canada), AF(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AG(Department of Geological &amp; Environmental Sciences, Stanford University; Air Products and Chemicals, Inc. Allentown), AH(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AI(Department of Biochemistry, Stanford University), AJ(Department of Chemistry, Stanford University; Department of Biochemistry, Stanford University), AK(Department of Biochemistry, Stanford University; Department of Biochemistry, Molecular Biology and Cell Biology, Northwestern University), AL(Department of Chemistry, Stanford University; , Institute for Research in Biomedicine), AM(Stanford Genome Technology Center, Stanford University; Department of Biochemistry, Stanford University), AN(Stanford Magnetic Resonance Laboratory, Stanford University; Department of Structural Biology, Stanford University), AO(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University), AP(Department of Geological &amp; Environmental Sciences, Stanford University), AQ(Department of Molecular and Cellular Physiology, Stanford University; Department of Structural Biology, Stanford University)\nBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\nJan 2009\n65\n\nPhysics\n\n(c) 2009: Springer Netherlands\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/abstract\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/toc\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2009bcet.book...65L/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nThe discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism. <P />\n10.1007/978-90-481-2368-1_5\n\n\n\n2007AAS...210.2104M\nTime Domain Exploration with the Palomar-QUEST Sky Survey\nMahabal, Ashish A.\nDrake, A. J.\nDjorgovski, S. G.\nDonalek, C.\nGlikman, E.\nGraham, M. J.\nWilliams, R.\nBaltay, C.\nRabinowitz, D.\nPQ Team Caltech\nYale\nNCSA\nIndiana\n, . . .\nAA(Caltech), AB(Caltech), AC(Caltech), AD(Caltech), AE(Caltech), AF(Caltech), AG(Caltech), AH(Yale University), AI(Yale University)\nAmerican Astronomical Society Meeting 210, id.21.04\n210\nMay 2007\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2007AAS...210.2104M/abstract\n\n\nTable of Contents\nhttps://ui.adsabs.harvard.edu/link_gateway/2007AAS...210.2104M/toc\n\nhttps://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nPalomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system. <P />Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys. <P />We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment. <P />The PQ survey is partially supported by the U.S. National Science Foundation (NSF). <P />\n\n\n\n2007RJPh....1...35.\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n., S. N. Agbo\n., E. C. Okoroigwe\nResearch Journal of Physics, vol. 1, issue 1, pp. 35-41\n1\nJan 2007\n35\n41\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2007RJPh....1...35./abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2007RJPh....1...35./PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nNot Available <P />\n10.3923/rjp.2007.35.41\n\n\n\n1995ans..agar..390M\nSpacecraft navigation requirements\nMiller, Judy L.\nAA(Draper (Charles Stark) Lab., Inc., Cambridge, MA.)\nIn AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\nJun 1995\n390\n405\n\nEarth Orbits\nNavigation Aids\nNavigators\nOnboard Equipment\nSpace Navigation\nSpacecraft Trajectories\nSupport Systems\nTechnology Assessment\nTechnology Utilization\nAscent Trajectories\nReentry Trajectories\nSpacecraft\nSpacecraft Performance\nSpacecraft Survivability\nTradeoffs\nWeight (Mass)\nSpace Communications, Spacecraft Communications, Command and Tracking\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1995ans..agar..390M/abstract\n\nhttps://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nSpacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy). <P />\n\n\n\n1995anda.book.....N\nApplied nonlinear dynamics: analytical, computational and experimental methods\nNayfeh, Ali H.\nBalachandran, Balakumar\nWiley series in nonlinear science, New York; Chichester: Wiley, |c1995\nJan 1995\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/citations\n118\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/1995anda.book.....N/coreads\n\nhttps://ui.adsabs.harvard.edu/abs/1995anda.book.....N\n118\nNot Available <P />\n\n\n\n1991hep.th....8028G\nApplied Conformal Field Theory\nGinsparg, Paul\neprint arXiv:hep-th/9108028\nNov 1988\n\nHigh Energy Physics - Theory\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/citations\n190\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/coreads\n\n\narXiv Article\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/EPRINT_HTML\n\n\narXiv PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/1991hep.th....8028G/EPRINT_PDF\n\nhttps://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\n190\nThese lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications <P />\narXiv:hep-th/9108028\n\n\n\n1983aiaa.meetY....K\nAutonomous navigation using lunar beacons\nKhatib, A. R.\nEllis, J.\nFrench, J.\nNull, G.\nYunck, T.\nWu, S.\nAA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)\nAmerican Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\nJan 1983\n\nArtificial Satellites\nAutonomous Navigation\nEarth-Moon System\nLunar Communication\nRadio Beacons\nRadio Navigation\nSpace Navigation\nDoppler Navigation\nLeast Squares Method\nOrbit Calculation\nSpace Communications, Spacecraft Communications, Command and Tracking\n\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/1983aiaa.meetY....K/abstract\n\nhttps://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nThe concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation. <P />\n\n\n\n2012ddsw.rept.....T\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nThornton, P. E.\nThornton, M. M.\nMayer, B. W.\nWilhelmi, N.\nWei, Y.\nDevarakonda, R.\nCook, R.\nOak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\nApr 2012\n\nDaymet\n\nOak Ridge National Laboratory\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/abstract\n\n\nCitations to the Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/citations\n51\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/coreads\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2012ddsw.rept.....T/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\n51\nArchived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\n10.3334/ORNLDAAC/1219\n\n\n\n2020EPJC...80...96D\nGeneralized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nDhaygude, Akanksha\nDesai, Shantanu\nAA(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India), AB(Department of Physics, IIT Hyderabad, 502285, Kandi, Telangana, India ;)\nThe European Physical Journal C, Volume 80, Issue 2, article id.96\nFeb 2020\n\nAstrophysics - High Energy Astrophysical Phenomena\nAstrophysics - Instrumentation and Methods for Astrophysics\nNuclear Experiment\n\n© The Author(s) 2020\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/coreads\n\n\narXiv Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/EPRINT_HTML\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/PUB_HTML\n\n\narXiv PDF\nhttps://ui.adsabs.harvard.edu/link_gateway/2020EPJC...80...96D/EPRINT_PDF\n\nhttps://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\nRecently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\n10.1140/epjc/s10052-020-7683-610.48550/arXiv.1912.06970\narXiv:1912.06970\n\n\n'} data_ref_with_abs_publisher = {'msg': 'Retrieved 5 abstracts, starting with number 1.', 'export': '\n\n\n2024zndo..10908474S\npc2/pqdts: v2024.2\nSchade, Robert\nAA(Paderborn Center for Parallel Computing @DCM-UPB)\nZenodo\nApr 2024\nZenodo\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2024zndo..10908474S/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2024zndo..10908474S/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2024zndo..10908474S\nChanges: improved installation mechanism for Julia spelling fixes in README.MD\n10.5281/zenodo.10908474\n\n\n\n2024wsp..conf...20V\nA modern view of former rivers on Mars.\nVidmachenko, A.\nAA(National University of Life and Environmental Sciences of Ukraine)\nProceedings of the VIII International Scientific and Practical Conference. World science priorities (February 08 – 09, 2024) Chapter Astronomy. Publisher: «World of Conferences». Vienna. Austria. P. 20-25. ISBN 978-92-44513-88-0.\nFeb 2024\n20\n25\n\nMars\nriverbeds\nmeandering valleys\nglaciers\neternal permafrost\n\nWorld of Conferences\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2024wsp..conf...20V/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2024wsp..conf...20V/coreads\n\n\nAuthor Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2024wsp..conf...20V/AUTHOR_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2024wsp..conf...20V\nNow the surface of Mars is a waterless desert, over which storms rage, raising sand and dust to a height of tens of kilometers. Under modern conditions, open bodies of water cannot exist on Mars. And water on the planet is contained either in the soil layer as permafrost, or in the form of open ice and snow; a very small amount of water is present in gaseous form in the atmosphere. The large reservoirs of water ice on Mars are the polar caps. Studies of Mars by spacecraft have shown that there is a huge amount of ice, and possibly liquid water, under the surface layer at a shallow depth. Analysis of the collected data allowed us to come to the conclusion that liquid water existed in significant quantities on the surface of Mars several billion years ago. That is, in the past, Mars had a full-fledged hydrosphere and a rather powerful atmosphere with a pressure near the surface of more than 0.4 bar. Later, the planet\'s climate changed. It lost much of its atmosphere and water, turning into a cold world. On the surface of Mars, there are numerous winding valleys with a long length, reminiscent of the dried-up channels of terrestrial rivers. A significant portion of the water that once flowed along currently dry riverbeds must now be under the surface of the planet. It is also possible that some channels are the result of the action of not liquid water, but a mixture of mud, ice and steam that flow only episodically. It is possible that the meandering valleys formed moving masses of glaciers. There is every reason to believe that there is still a lot of water on Mars, and it still exists in the form of permafrost. A perspective image of the Echus Chasma region suggests that liquid water was present on this part of the Martian surface up to a billion years ago. Later, the planet cooled down, the lakes froze, and glaciers formed, which \'cut\' the Kasei Valles with their streams.\n\n\n\n2024asal.book..204V\nNew generation telescopes for the astronomy of the future.\nVidmachenko, A.\nAA(National University of Life and Environmental Sciences of Ukraine)\nIn book: Astronomical almanac, 70, Edition: MAO NAS of Ukraine. Publisher: Kyiv, Akademperiodika, p. 204-209.\nJan 2024\n204\n209\n\nnew astronomical instruments\nTelescopes\ntelescope construction\nastronomical research\n\nKyiv\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2024asal.book..204V/abstract\n\n\nCo-Reads\nhttps://ui.adsabs.harvard.edu/link_gateway/2024asal.book..204V/coreads\n\n\nAuthor Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2024asal.book..204V/AUTHOR_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2024asal.book..204V\nIn the next few years, several new astronomical instruments are planned to be launched on Earth and in space. Each of these devices is very expensive! But many countries allocate large amounts of money for this, and plan to receive more and more recent data about the surrounding universe. Telescopes are devices for observing distant objects. The very first working telescope was created in 1608 by the Dutch optician Hans Lippersgei. The creation of the telescope was also attributed to such masters as another Dutch eyeglass maker from Middelburg, Zachary Janssen, and Jacob Mathews from the city of Alkmaar. These earliest telescopes consisted of a convex lens as an objective and a concave lens that served as an eyepiece. In 1609, Galileo Galilei significantly improved the design of the telescope, achieving a 30-fold increase in the original images. With its help, Galileo performed the first survey of the heavenly bodies. Therefore, even now, the creation of astronomical instruments, whose characteristics significantly improve previous examples of telescope construction, is considered extremely important in astronomical research. The Hubble telescope was the first to provide interesting information about the features of images of the most distant galaxies. They are significantly different from those formed relatively recently. One of the world\'s largest ground-based telescopes, the Giant Magellan Telescope, is under construction. It is being built in Chile and its gradual commissioning will begin in 2024. Segments of seven monolithic mirrors, with a diameter of 8.4 m each, create an optical surface with an equivalent diameter of 24.5 m. Larger will be the 30-meter telescope, which is planned to be built on the island of Hawaii, next to the two 9-meter Keck reflectors at the Mauna Kea observatory. The mirror surface of this telescope will consist of almost five hundred hexagonal segments and will reach a diameter of 30 m. It is expected to be tested in 2027. In 2014, the European Southern Observatory started the construction of the Extremely Large Telescope. In 2025, it is planned to become the most powerful optical astronomical instrument in the world, with an equivalent diameter of its mirror surface of 39 m.\n\n\n\n2018scrp.conf.....K\nScience and Computing with Raspberry Pi\nKent, Brian R.\nAA(NRAO)\nScience and Computing with Raspberry Pi, by Brian R. Kent. Online ISBN: 978-1-6817-4996-9, Print ISBN: 978-1-6817-4993-8, Morgan &amp; Claypool Publishers, 2018\nJul 2018\n\nsingle board computing\nastronomy\nvery large array\nastrophysics\nvisualization\ndata science\ncomputing\nradio astronomy\n\nMorgan & Claypool\nCopyright (c) 2018 Morgan & Claypool Publishers\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2018scrp.conf.....K/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2018scrp.conf.....K/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2018scrp.conf.....K\nThe portable Raspberry Pi computing platform with the power of Linux yields an exciting exploratory tool for beginning scientific computing. Science and Computing with Raspberry Pi takes the reader through explorations in a variety of computing exercises with the physical sciences. The book guides the user through: configuring your Raspberry Pi and Linux operating system; understanding the software requirements while using the Pi for scientific computing; computing exercises in physics, astronomy, chaos theory, and machine learning.\n\n\n\n2023uwff.book.....R\nUnder the weather: a future forecast for New Zealand\nRenwick, J. A.\nUnder the weather: a future forecast for New Zealand, by J. A. Renwick, 2023. Auckland: HarperCollins Publishers. OCLC: 1388369161. ISBN: 9781775541721.\nJan 2023\nHarperCollins\n\nabstract\nhttps://ui.adsabs.harvard.edu/link_gateway/2023uwff.book.....R/abstract\n\n\nPublisher Article\nhttps://ui.adsabs.harvard.edu/link_gateway/2023uwff.book.....R/PUB_HTML\n\nhttps://ui.adsabs.harvard.edu/abs/2023uwff.book.....R\nA forecast for New Zealand\'s changing climate and why it matters to our everyday lives A warmer world will change more than just our weather patterns. It will change the look of the land around us, what grows and lives on it - including us. Drawing on climate models that can travel to ice ages and hothouses of the deep past, Professor James Renwick untangles how we know exactly what the future holds and why it matters to our everyday lives. He looks at New Zealand\'s more frequent natural disasters, warming and increasingly acidic waters, the creep of rising sea levels, and the ways that the changing weather will affect our agriculture, lifestyle, food security and economy.Arresting, galvanizing and clear-sighted, Under the Weather is a picture of a miraculous planet in danger, a stock-take on what it means for this small country, and a reminder that the shape of our future is up to us.\'--Publisher description.\n\n\n'} -data_jats = {'msg': 'Retrieved 23 abstracts, starting with number 1.', 'export': '\n\n\n

\n\n\nWthr\n0043-1656\n\n\n2018Wthr...73Q..35.\n10.1002/wea.3072\n\nBook reviews\n\n\n\n00\n01\n2018\n\n73\n1\n35\n35\n\n\n

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\n\n\nTDM\n2053-1583\n\n\n2018TDM.....5a0201F\n10.1088/2053-1583/aa9403\n\n2D Materials: maintaining editorial quality\n\n\n\n00\n01\n2018\n\n5\n1\n\n\n

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\n\n\nSpin\n\n\n2018Spin....877001P\n10.1142/S2010324718770015\n\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\n\n\n\n00\n00\n2018\n\n8\n4\n\n\n

Not Available <P />

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\n\n\nSAAS\n\n\n2018SAAS...38.....D\n10.1007/978-3-662-57546-8\n\nMillimeter Astronomy\n\n\n\n00\n00\n2018\n\n38\n\n\n

Not Available <P />

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\n\n\nPhRvL\n0031-9007\n\n\n2018PhRvL.120b9901P\n10.1103/PhysRevLett.120.029901\n\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\n\n\n\n00\n01\n2018\n\n120\n2\n\n\n

Not Available <P />

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\n\n\nPhDT\n\n\n2017PhDT........14C\n10.5281/zenodo.581221\n\nResolving Gas-Phase Metallicity In Galaxies\n\n\n\n00\n06\n2017\n\n\n\n

Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation. <P />Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies. <P />Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient. <P />Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas. <P />

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\n\n\nnova\n\n\n2017nova.pres.2388K\n\nA 3D View of a Supernova Remnant\n\n\n\n00\n06\n2017\n\n\n\n

The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384 <P />

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\n\n\nCBET\n\n\n2017CBET.4403....2G\n\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\n\n\n\n00\n06\n2017\n\n4403\n2\n\n\n

A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg). <P />

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\n\n\nascl\n\n\n2017ascl.soft06009C\n\nsick: Spectroscopic inference crank\n\n\n\n00\n06\n2017\n\n\n\n

sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data. <P />

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\n\n\nyCat\n\n\n2017yCat.113380453S\n\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\n\n\n\n00\n05\n2017\n\n\n\n

The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star. <P />The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />

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\n\n\nAAVSN\n\n\n2017AAVSN.429....1W\n\nV694 Mon (MWC 560) spectroscopy requested\n\n\n\n00\n05\n2017\n\n429\n1\n\n\n

The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details. <P />

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\n\n\nsptz\n\n\n2017sptz.prop13168Y\n\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\n\n\n\n00\n04\n2017\n\n13168\n\n\n

ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event. <P />

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\n\n\nMsT\n\n\n2017MsT..........2A\n\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\n\n\n\n00\n03\n2017\n\n2\n\n\n

The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads. <P />

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\n\n\nemo6\n\n\n2016emo6.rept.....R\n\nThe penumbral Moon\'s eclipse form 16 september 2016\n\n\n\n00\n10\n2016\n\n\n\n

The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon. <P />

\n\n\n\n
\n
\n\n\niac\n\n\n2016iac..talk..872V\n\nLiving on the edge: Adaptive Optics+Lucky Imaging\n\n\n\n00\n03\n2016\n\n872\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nbcet\n\n\n2009bcet.book...65L\n10.1007/978-90-481-2368-1_5\n\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\n\n\n\n00\n00\n2009\n\n65\n\n\n

The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism. <P />

\n\n\n\n
\n
\n\n\nAAS\n\n\n2007AAS...210.2104M\n\nTime Domain Exploration with the Palomar-QUEST Sky Survey\n\n\n\n00\n05\n2007\n\n210\n\n\n

Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system. <P />Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys. <P />We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment. <P />The PQ survey is partially supported by the U.S. National Science Foundation (NSF). <P />

\n\n\n\n
\n
\n\n\nRJPh\n1819-3463\n\n\n2007RJPh....1...35.\n10.3923/rjp.2007.35.41\n\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n\n\n\n00\n01\n2007\n\n1\n1\n35\n41\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nans\n\n\n1995ans..agar..390M\n\nSpacecraft navigation requirements\n\n\n\n00\n06\n1995\n\n390\n405\n\n\n

Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy). <P />

\n\n\n\n
\n
\n\n\nanda\n\n\n1995anda.book.....N\n\nApplied nonlinear dynamics: analytical, computational and experimental methods\n\n\n\n00\n00\n1995\n\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\narXiv\n\n\n1991hep.th....8028G\n\nApplied Conformal Field Theory\n\n\n\n00\n11\n1988\n\n\n\n

These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications <P />

\n\n\n\n
\n
\n\n\naiaa\n\n\n1983aiaa.meetY....K\n\nAutonomous navigation using lunar beacons\n\n\n\n00\n01\n1983\n\n\n\n

The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation. <P />

\n\n\n\n
\n
\n\n\nddsw\n\n\n2012ddsw.rept.....T\n10.3334/ORNLDAAC/1219\n\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\n\n\n\n00\n04\n2012\n\n\n\n

Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.

\n\n\n\n
\n'} +data_jats = {'msg': 'Retrieved 24 abstracts, starting with number 1.', 'export': '\n\n\n
\n\n\nWthr\n0043-1656\n\n\n2018Wthr...73Q..35.\n10.1002/wea.3072\n\nBook reviews\n\n\n\n00\n01\n2018\n\n73\n1\n35\n35\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nTDM\n2053-1583\n\n\n2018TDM.....5a0201F\n10.1088/2053-1583/aa9403\n\n2D Materials: maintaining editorial quality\n\n\n\n00\n01\n2018\n\n5\n1\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nSpin\n\n\n2018Spin....877001P\n10.1142/S2010324718770015\n\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\n\n\n\n00\n00\n2018\n\n8\n4\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nSAAS\n\n\n2018SAAS...38.....D\n10.1007/978-3-662-57546-8\n\nMillimeter Astronomy\n\n\n\n00\n00\n2018\n\n38\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nPhRvL\n0031-9007\n\n\n2018PhRvL.120b9901P\n10.1103/PhysRevLett.120.029901\n\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\n\n\n\n00\n01\n2018\n\n120\n2\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nPhDT\n\n\n2017PhDT........14C\n10.5281/zenodo.581221\n\nResolving Gas-Phase Metallicity In Galaxies\n\n\n\n00\n06\n2017\n\n\n\n

Chapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-\'normal\' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation. <P />Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies. <P />Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient. <P />Chapter 5 The relationship between a galaxy\'s stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas. <P />

\n\n\n\n
\n
\n\n\nnova\n\n\n2017nova.pres.2388K\n\nA 3D View of a Supernova Remnant\n\n\n\n00\n06\n2017\n\n\n\n

The outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384 <P />

\n\n\n\n
\n
\n\n\nCBET\n\n\n2017CBET.4403....2G\n\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\n\n\n\n00\n06\n2017\n\n4403\n2\n\n\n

A previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg). <P />

\n\n\n\n
\n
\n\n\nascl\n\n\n2017ascl.soft06009C\n\nsick: Spectroscopic inference crank\n\n\n\n00\n06\n2017\n\n\n\n

sick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data. <P />

\n\n\n\n
\n
\n\n\nyCat\n\n\n2017yCat.113380453S\n\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\n\n\n\n00\n05\n2017\n\n\n\n

The included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star. <P />The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />

\n\n\n\n
\n
\n\n\nAAVSN\n\n\n2017AAVSN.429....1W\n\nV694 Mon (MWC 560) spectroscopy requested\n\n\n\n00\n05\n2017\n\n429\n1\n\n\n

The observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details. <P />

\n\n\n\n
\n
\n\n\nsptz\n\n\n2017sptz.prop13168Y\n\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\n\n\n\n00\n04\n2017\n\n13168\n\n\n

ULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event. <P />

\n\n\n\n
\n
\n\n\nMsT\n\n\n2017MsT..........2A\n\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\n\n\n\n00\n03\n2017\n\n2\n\n\n

The African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads. <P />

\n\n\n\n
\n
\n\n\nemo6\n\n\n2016emo6.rept.....R\n\nThe penumbral Moon\'s eclipse form 16 september 2016\n\n\n\n00\n10\n2016\n\n\n\n

The web page represents circumstances and photographs from the Moon\'s partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon. <P />

\n\n\n\n
\n
\n\n\niac\n\n\n2016iac..talk..872V\n\nLiving on the edge: Adaptive Optics+Lucky Imaging\n\n\n\n00\n03\n2016\n\n872\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nbcet\n\n\n2009bcet.book...65L\n10.1007/978-90-481-2368-1_5\n\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\n\n\n\n00\n00\n2009\n\n65\n\n\n

The discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism. <P />

\n\n\n\n
\n
\n\n\nAAS\n\n\n2007AAS...210.2104M\n\nTime Domain Exploration with the Palomar-QUEST Sky Survey\n\n\n\n00\n05\n2007\n\n210\n\n\n

Palomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system. <P />Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys. <P />We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment. <P />The PQ survey is partially supported by the U.S. National Science Foundation (NSF). <P />

\n\n\n\n
\n
\n\n\nRJPh\n1819-3463\n\n\n2007RJPh....1...35.\n10.3923/rjp.2007.35.41\n\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n\n\n\n00\n01\n2007\n\n1\n1\n35\n41\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\nans\n\n\n1995ans..agar..390M\n\nSpacecraft navigation requirements\n\n\n\n00\n06\n1995\n\n390\n405\n\n\n

Spacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy). <P />

\n\n\n\n
\n
\n\n\nanda\n\n\n1995anda.book.....N\n\nApplied nonlinear dynamics: analytical, computational and experimental methods\n\n\n\n00\n00\n1995\n\n\n\n

Not Available <P />

\n\n\n\n
\n
\n\n\narXiv\n\n\n1991hep.th....8028G\n\nApplied Conformal Field Theory\n\n\n\n00\n11\n1988\n\n\n\n

These lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications <P />

\n\n\n\n
\n
\n\n\naiaa\n\n\n1983aiaa.meetY....K\n\nAutonomous navigation using lunar beacons\n\n\n\n00\n01\n1983\n\n\n\n

The concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon\'s surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation. <P />

\n\n\n\n
\n
\n\n\nddsw\n\n\n2012ddsw.rept.....T\n10.3334/ORNLDAAC/1219\n\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\n\n\n\n00\n04\n2012\n\n\n\n

Archived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.

\n\n\n\n
\n
\n\n\nEPJC\n\n\n2020EPJC...80...96D\n10.1140/epjc/s10052-020-7683-6; 10.48550/arXiv.1912.06970\n\nGeneralized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\n\n\n\n00\n02\n2020\n\n\n\n

Recently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.

\n\n\n\n
\n'} data_jats_one_record = {'msg': 'Retrieved 1 abstracts, starting with number 1.', 'export': '\n\n
\n\n\nAAS\n\n\n2018AAS...23221409A\n\nThe NASA Astrophysics Data System: Capabilities and Roadmap for the 2020s\n\n\n\n\nAccomazzi\nAlberto\n\nHarvard Smithsonian, CfA\n\n\n\nADS Team\n\n\n\n\n00\n06\n2018\n\n232\n\n\n

The NASA Astrophysics Data System (ADS) is used daily by researchers and curators as a discovery platform for the Astronomy literature. Over the past several years, the ADS has been adding to the breadth and depth of its contents. Scholarly astronomy articles are now indexed as full-text documents, allowing for complete and accurate literature searches. High-level data products, data links, and software used in refereed astronomy papers are now also being ingested and indexed in our database. All the search functionality exposed in the new ADS interface is also available via its API, which we are continuing to develop and enhance. In this talk I will describe the current system, our current roadmap, and solicit input from the community regarding what additional data, services, and discovery capabilities the ADS should support.

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'} data_jats_publisher = {'msg': 'Retrieved 5 abstracts, starting with number 1.', 'export': '\n\n\n
\n\n\nzndo\n\nZenodo\n\n\n\n2024zndo..10908474S\n10.5281/zenodo.10908474\n\npc2/pqdts: v2024.2\n\n\n\n02\n04\n2024\n\n\n\n

Changes: improved installation mechanism for Julia spelling fixes in README.MD

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\n
\n\n\nwsp\n\nWorld of Conferences\n\n\n\n2024wsp..conf...20V\n\nA modern view of former rivers on Mars.\n\n\n\n0000-0002-0523-5234\n\nVidmachenko\nA.\n\nNational University of Life and Environmental Sciences of Ukraine\n\n\n\n00\n02\n2024\n\n20\n25\n\n\n

Now the surface of Mars is a waterless desert, over which storms rage, raising sand and dust to a height of tens of kilometers. Under modern conditions, open bodies of water cannot exist on Mars. And water on the planet is contained either in the soil layer as permafrost, or in the form of open ice and snow; a very small amount of water is present in gaseous form in the atmosphere. The large reservoirs of water ice on Mars are the polar caps. Studies of Mars by spacecraft have shown that there is a huge amount of ice, and possibly liquid water, under the surface layer at a shallow depth. Analysis of the collected data allowed us to come to the conclusion that liquid water existed in significant quantities on the surface of Mars several billion years ago. That is, in the past, Mars had a full-fledged hydrosphere and a rather powerful atmosphere with a pressure near the surface of more than 0.4 bar. Later, the planet\'s climate changed. It lost much of its atmosphere and water, turning into a cold world. On the surface of Mars, there are numerous winding valleys with a long length, reminiscent of the dried-up channels of terrestrial rivers. A significant portion of the water that once flowed along currently dry riverbeds must now be under the surface of the planet. It is also possible that some channels are the result of the action of not liquid water, but a mixture of mud, ice and steam that flow only episodically. It is possible that the meandering valleys formed moving masses of glaciers. There is every reason to believe that there is still a lot of water on Mars, and it still exists in the form of permafrost. A perspective image of the Echus Chasma region suggests that liquid water was present on this part of the Martian surface up to a billion years ago. Later, the planet cooled down, the lakes froze, and glaciers formed, which \'cut\' the Kasei Valles with their streams.

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\n\n\nasal\n\nKyiv\n\n\n\n2024asal.book..204V\n\nNew generation telescopes for the astronomy of the future.\n\n\n\n0000-0002-0523-5234\n\nVidmachenko\nA.\n\nNational University of Life and Environmental Sciences of Ukraine\n\n\n\n00\n01\n2024\n\n204\n209\n\n\n

In the next few years, several new astronomical instruments are planned to be launched on Earth and in space. Each of these devices is very expensive! But many countries allocate large amounts of money for this, and plan to receive more and more recent data about the surrounding universe. Telescopes are devices for observing distant objects. The very first working telescope was created in 1608 by the Dutch optician Hans Lippersgei. The creation of the telescope was also attributed to such masters as another Dutch eyeglass maker from Middelburg, Zachary Janssen, and Jacob Mathews from the city of Alkmaar. These earliest telescopes consisted of a convex lens as an objective and a concave lens that served as an eyepiece. In 1609, Galileo Galilei significantly improved the design of the telescope, achieving a 30-fold increase in the original images. With its help, Galileo performed the first survey of the heavenly bodies. Therefore, even now, the creation of astronomical instruments, whose characteristics significantly improve previous examples of telescope construction, is considered extremely important in astronomical research. The Hubble telescope was the first to provide interesting information about the features of images of the most distant galaxies. They are significantly different from those formed relatively recently. One of the world\'s largest ground-based telescopes, the Giant Magellan Telescope, is under construction. It is being built in Chile and its gradual commissioning will begin in 2024. Segments of seven monolithic mirrors, with a diameter of 8.4 m each, create an optical surface with an equivalent diameter of 24.5 m. Larger will be the 30-meter telescope, which is planned to be built on the island of Hawaii, next to the two 9-meter Keck reflectors at the Mauna Kea observatory. The mirror surface of this telescope will consist of almost five hundred hexagonal segments and will reach a diameter of 30 m. It is expected to be tested in 2027. In 2014, the European Southern Observatory started the construction of the Extremely Large Telescope. In 2025, it is planned to become the most powerful optical astronomical instrument in the world, with an equivalent diameter of its mirror surface of 39 m.

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\n\n\nscrp\n\nMorgan & Claypool\n\n\n\n2018scrp.conf.....K\n\nScience and Computing with Raspberry Pi\n\n\n\n\nKent\nBrian R.\n\nNRAO\n\n\n\n00\n07\n2018\n\n\n\n

The portable Raspberry Pi computing platform with the power of Linux yields an exciting exploratory tool for beginning scientific computing. Science and Computing with Raspberry Pi takes the reader through explorations in a variety of computing exercises with the physical sciences. The book guides the user through: configuring your Raspberry Pi and Linux operating system; understanding the software requirements while using the Pi for scientific computing; computing exercises in physics, astronomy, chaos theory, and machine learning.

\n\n\n\n
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\n\n\nuwff\n\nHarperCollins\n\n\n\n2023uwff.book.....R\n\nUnder the weather: a future forecast for New Zealand\n\n\n\n\nRenwick\nJ. A.\n\n\n\n\n00\n00\n2023\n\n\n\n

A forecast for New Zealand\'s changing climate and why it matters to our everyday lives A warmer world will change more than just our weather patterns. It will change the look of the land around us, what grows and lives on it - including us. Drawing on climate models that can travel to ice ages and hothouses of the deep past, Professor James Renwick untangles how we know exactly what the future holds and why it matters to our everyday lives. He looks at New Zealand\'s more frequent natural disasters, warming and increasingly acidic waters, the creep of rising sea levels, and the ways that the changing weather will affect our agriculture, lifestyle, food security and economy.Arresting, galvanizing and clear-sighted, Under the Weather is a picture of a miraculous planet in danger, a stock-take on what it means for this small country, and a reminder that the shape of our future is up to us.\'--Publisher description.

\n\n\n\n
\n'} -data_dublin_core_individual = {'num_docs': 23, 'docs': [{'bibcode': '2018Wthr...73Q..35.', 'reference': '\n2018Wthr...73Q..35.\nBook reviews\nWeather, vol. 73, issue 1, pp. 35-35\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nNot Available <P />\ndoi:10.1002/wea.3072\n\n\n'}, {'bibcode': '2018TDM.....5a0201F', 'reference': "\n2018TDM.....5a0201F\n2D Materials: maintaining editorial quality\nFal'ko, Vladimir\nThomas, Ceri-Wyn\n2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nNot Available <P />\ndoi:10.1088/2053-1583/aa9403\n\n\n"}, {'bibcode': '2018Spin....877001P', 'reference': '\n2018Spin....877001P\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nParkin, Stuart\nChantrell, Roy\nChang, Ching-Ray\nSpin, Volume 8, Issue 4, id. 1877001\n2018-01-01\n(c) 2018: World Scientific Publishing Company\nhttps://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nNot Available <P />\ndoi:10.1142/S2010324718770015\n\n\n'}, {'bibcode': '2018SAAS...38.....D', 'reference': '\n2018SAAS...38.....D\nMillimeter Astronomy\nDessauges-Zavadsky, Miroslava\nPfenniger, Daniel\nMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\n2018-01-01\nPhysics\n(c) 2018: Springer-Verlag GmbH Germany, part of Springer Nature\nhttps://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nNot Available <P />\ndoi:10.1007/978-3-662-57546-8\n\n\n'}, {'bibcode': '2018PhRvL.120b9901P', 'reference': '\n2018PhRvL.120b9901P\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nPustilnik, M.\nvan Heck, B.\nLutchyn, R. M.\nGlazman, L. I.\nPhysical Review Letters, Volume 120, Issue 2, id.029901\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nNot Available <P />\ndoi:10.1103/PhysRevLett.120.029901\n\n\n'}, {'bibcode': '2017PhDT........14C', 'reference': "\n2017PhDT........14C\nResolving Gas-Phase Metallicity In Galaxies\nCarton, David\nPhD Thesis, Leiden University, 2017\n2017-06-01\ngalaxies: evolution, galaxies: abundances, galaxies: ISM\nhttps://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nChapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-'normal' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation. <P />Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies. <P />Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient. <P />Chapter 5 The relationship between a galaxy's stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas. <P />\ndoi:10.5281/zenodo.581221\n\n\n"}, {'bibcode': '2017nova.pres.2388K', 'reference': '\n2017nova.pres.2388K\nA 3D View of a Supernova Remnant\nKohler, Susanna\nAAS Nova Highlight, 14 Jun 2017, id.2388\n2017-06-01\nFeatures, Highlights, interstellar medium, stellar evolution, supernova remnant, supernovae, white dwarfs\nhttps://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nThe outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384 <P />\n\n\n'}, {'bibcode': '2017CBET.4403....2G', 'reference': '\n2017CBET.4403....2G\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\nGreen, D. W. E.\nCentral Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\n2017-06-01\nhttps://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nA previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg). <P />\n\n\n'}, {'bibcode': '2017ascl.soft06009C', 'reference': '\n2017ascl.soft06009C\nsick: Spectroscopic inference crank\nCasey, Andrew R.\nAstrophysics Source Code Library, record ascl:1706.009\n2017-06-01\nSoftware\nhttps://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nsick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data. <P />\n\n\n'}, {'bibcode': '2017yCat.113380453S', 'reference': '\n2017yCat.113380453S\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nSiltala, J.\nJetsu, L.\nHackman, T.\nHenry, G. W.\nImmonen, L.\nKajatkari, P.\nLankinen, J.\nLehtinen, J.\nMonira, S.\nNikbakhsh, S.\nViitanen, A.\nViuho, J.\nWillamo, T.\nVizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\n2017-05-01\nStars: variable\nhttps://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nThe included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star. <P />The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />\n\n\n'}, {'bibcode': '2017AAVSN.429....1W', 'reference': '\n2017AAVSN.429....1W\nV694 Mon (MWC 560) spectroscopy requested\nWaagen, Elizabeth O.\nAAVSO Special Notice #429\n2017-05-01\nastronomical databases: miscellaneous, binaries: symbiotic, stars: individual (V694 Mon, MWC 560)\n(C) AAVSO 2017\nhttps://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nThe observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details. <P />\n\n\n'}, {'bibcode': '2017sptz.prop13168Y', 'reference': '\n2017sptz.prop13168Y\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nYan, Lin\nSpitzer Proposal ID 13168\n2017-04-01\nhttps://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event. <P />\n\n\n'}, {'bibcode': '2017MsT..........2A', 'reference': '\n2017MsT..........2A\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAzankpo, Severin\nMasters thesis, University of Stellenbosch, March 2017, 120 pages\n2017-03-01\nhttps://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nThe African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads. <P />\n\n\n'}, {'bibcode': '2016emo6.rept.....R', 'reference': "\n2016emo6.rept.....R\nThe penumbral Moon's eclipse form 16 september 2016\nRotaru, Adrian\nPteancu, Mircea\nZaharia, Cristian\nhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\n2016-10-01\nTHE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY\nhttps://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nThe web page represents circumstances and photographs from the Moon's partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon. <P />\n\n\n"}, {'bibcode': '2016iac..talk..872V', 'reference': '\n2016iac..talk..872V\nLiving on the edge: Adaptive Optics+Lucky Imaging\nVelasco, Sergio\nIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\n2016-03-01\nhttps://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nNot Available <P />\n\n\n'}, {'bibcode': '2009bcet.book...65L', 'reference': '\n2009bcet.book...65L\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\nLiu, Corey W.\nAlekseyev, Viktor Y.\nAllwardt, Jeffrey R.\nBankovich, Alexander J.\nCade-Menun, Barbara J.\nDavis, Ronald W.\nDu, Lin-Shu\nGarcia, K. Christopher\nHerschlag, Daniel\nKhosla, Chaitan\nKraut, Daniel A.\nLi, Qing\nNull, Brian\nPuglisi, Joseph D.\nSigala, Paul A.\nStebbins, Jonathan F.\nVarani, Luca\nBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\n2009-01-01\nPhysics\n(c) 2009: Springer Netherlands\nhttps://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nThe discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism. <P />\ndoi:10.1007/978-90-481-2368-1_5\n\n\n'}, {'bibcode': '2007AAS...210.2104M', 'reference': '\n2007AAS...210.2104M\nTime Domain Exploration with the Palomar-QUEST Sky Survey\nMahabal, Ashish A.\nDrake, A. J.\nDjorgovski, S. G.\nDonalek, C.\nGlikman, E.\nGraham, M. J.\nWilliams, R.\nBaltay, C.\nRabinowitz, D.\nPQ Team Caltech\nYale\nNCSA\nIndiana\n, . . .\nAmerican Astronomical Society Meeting 210, id.21.04\n2007-05-01\nhttps://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nPalomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system. <P />Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys. <P />We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment. <P />The PQ survey is partially supported by the U.S. National Science Foundation (NSF). <P />\n\n\n'}, {'bibcode': '2007RJPh....1...35.', 'reference': '\n2007RJPh....1...35.\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n., S. N. Agbo\n., E. C. Okoroigwe\nResearch Journal of Physics, vol. 1, issue 1, pp. 35-41\n2007-01-01\nhttps://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nNot Available <P />\ndoi:10.3923/rjp.2007.35.41\n\n\n'}, {'bibcode': '1995ans..agar..390M', 'reference': '\n1995ans..agar..390M\nSpacecraft navigation requirements\nMiller, Judy L.\nIn AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\n1995-06-01\nEarth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space Navigation, Spacecraft Trajectories, Support Systems, Technology Assessment, Technology Utilization, Ascent Trajectories, Reentry Trajectories, Spacecraft, Spacecraft Performance, Spacecraft Survivability, Tradeoffs, Weight (Mass), Space Communications, Spacecraft Communications, Command and Tracking\nhttps://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nSpacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy). <P />\n\n\n'}, {'bibcode': '1995anda.book.....N', 'reference': '\n1995anda.book.....N\nApplied nonlinear dynamics: analytical, computational and experimental methods\nNayfeh, Ali H.\nBalachandran, Balakumar\nWiley series in nonlinear science, New York; Chichester: Wiley, |c1995\n1995-01-01\nhttps://ui.adsabs.harvard.edu/abs/1995anda.book.....N\ncitations:118\nNot Available <P />\n\n\n'}, {'bibcode': '1991hep.th....8028G', 'reference': '\n1991hep.th....8028G\nApplied Conformal Field Theory\nGinsparg, Paul\neprint arXiv:hep-th/9108028\n1988-11-01\nHigh Energy Physics - Theory\nhttps://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\ncitations:190\nThese lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications <P />\n\n\n'}, {'bibcode': '1983aiaa.meetY....K', 'reference': "\n1983aiaa.meetY....K\nAutonomous navigation using lunar beacons\nKhatib, A. R.\nEllis, J.\nFrench, J.\nNull, G.\nYunck, T.\nWu, S.\nAmerican Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\n1983-01-01\nArtificial Satellites, Autonomous Navigation, Earth-Moon System, Lunar Communication, Radio Beacons, Radio Navigation, Space Navigation, Doppler Navigation, Least Squares Method, Orbit Calculation, Space Communications, Spacecraft Communications, Command and Tracking\nhttps://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nThe concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon's surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation. <P />\n\n\n"}, {'bibcode': '2012ddsw.rept.....T', 'reference': '\n2012ddsw.rept.....T\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nThornton, P. E.\nThornton, M. M.\nMayer, B. W.\nWilhelmi, N.\nWei, Y.\nDevarakonda, R.\nCook, R.\nOak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\n2012-04-01\nDaymet\nOak Ridge National Laboratory\nhttps://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\ncitations:51\nArchived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\ndoi:10.3334/ORNLDAAC/1219\n\n\n'}], 'header': '\n\n', 'footer': ''} +data_dublin_core_individual = {'num_docs': 24, 'docs': [{'bibcode': '2018Wthr...73Q..35.', 'reference': '\n2018Wthr...73Q..35.\nBook reviews\nWeather, vol. 73, issue 1, pp. 35-35\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018Wthr...73Q..35.\nNot Available <P />\ndoi:10.1002/wea.3072\n\n\n'}, {'bibcode': '2018TDM.....5a0201F', 'reference': "\n2018TDM.....5a0201F\n2D Materials: maintaining editorial quality\nFal'ko, Vladimir\nThomas, Ceri-Wyn\n2D Materials, Volume 5, Issue 1, article id. 010201 (2018).\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018TDM.....5a0201F\nNot Available <P />\ndoi:10.1088/2053-1583/aa9403\n\n\n"}, {'bibcode': '2018Spin....877001P', 'reference': '\n2018Spin....877001P\nObituary: In Memoriam Professor Dr. Shoucheng Zhang, Consulting Editor\nParkin, Stuart\nChantrell, Roy\nChang, Ching-Ray\nSpin, Volume 8, Issue 4, id. 1877001\n2018-01-01\n(c) 2018: World Scientific Publishing Company\nhttps://ui.adsabs.harvard.edu/abs/2018Spin....877001P\nNot Available <P />\ndoi:10.1142/S2010324718770015\n\n\n'}, {'bibcode': '2018SAAS...38.....D', 'reference': '\n2018SAAS...38.....D\nMillimeter Astronomy\nDessauges-Zavadsky, Miroslava\nPfenniger, Daniel\nMillimeter Astronomy: Saas-Fee Advanced Course 38. Swiss Society for Astrophysics and Astronomy, Saas-Fee Advanced Course, Volume 38. ISBN 978-3-662-57545-1. Springer-Verlag GmbH Germany, part of Springer Nature, 2018\n2018-01-01\nPhysics\n(c) 2018: Springer-Verlag GmbH Germany, part of Springer Nature\nhttps://ui.adsabs.harvard.edu/abs/2018SAAS...38.....D\nNot Available <P />\ndoi:10.1007/978-3-662-57546-8\n\n\n'}, {'bibcode': '2018PhRvL.120b9901P', 'reference': '\n2018PhRvL.120b9901P\nErratum: Quantum Criticality in Resonant Andreev Conduction [Phys. Rev. Lett. 119, 116802 (2017)]\nPustilnik, M.\nvan Heck, B.\nLutchyn, R. M.\nGlazman, L. I.\nPhysical Review Letters, Volume 120, Issue 2, id.029901\n2018-01-01\nhttps://ui.adsabs.harvard.edu/abs/2018PhRvL.120b9901P\nNot Available <P />\ndoi:10.1103/PhysRevLett.120.029901\n\n\n'}, {'bibcode': '2017PhDT........14C', 'reference': "\n2017PhDT........14C\nResolving Gas-Phase Metallicity In Galaxies\nCarton, David\nPhD Thesis, Leiden University, 2017\n2017-06-01\ngalaxies: evolution, galaxies: abundances, galaxies: ISM\nhttps://ui.adsabs.harvard.edu/abs/2017PhDT........14C\nChapter 2: As part of the Bluedisk survey we analyse the radial gas-phase metallicity profiles of 50 late-type galaxies. We compare the metallicity profiles of a sample of HI-rich galaxies against a control sample of HI-'normal' galaxies. We find the metallicity gradient of a galaxy to be strongly correlated with its HI mass fraction {M}{HI}) / {M}_{\\ast}). We note that some galaxies exhibit a steeper metallicity profile in the outer disc than in the inner disc. These galaxies are found in both the HI-rich and control samples. This contradicts a previous indication that these outer drops are exclusive to HI-rich galaxies. These effects are not driven by bars, although we do find some indication that barred galaxies have flatter metallicity profiles. By applying a simple analytical model we are able to account for the variety of metallicity profiles that the two samples present. The success of this model implies that the metallicity in these isolated galaxies may be in a local equilibrium, regulated by star formation. This insight could provide an explanation of the observed local mass-metallicity relation. <P />Chapter 3 We present a method to recover the gas-phase metallicity gradients from integral field spectroscopic (IFS) observations of barely resolved galaxies. We take a forward modelling approach and compare our models to the observed spatial distribution of emission line fluxes, accounting for the degrading effects of seeing and spatial binning. The method is flexible and is not limited to particular emission lines or instruments. We test the model through comparison to synthetic observations and use downgraded observations of nearby galaxies to validate this work. As a proof of concept we also apply the model to real IFS observations of high-redshift galaxies. From our testing we show that the inferred metallicity gradients and central metallicities are fairly insensitive to the assumptions made in the model and that they are reliably recovered for galaxies with sizes approximately equal to the half width at half maximum of the point-spread function. However, we also find that the presence of star forming clumps can significantly complicate the interpretation of metallicity gradients in moderately resolved high-redshift galaxies. Therefore we emphasize that care should be taken when comparing nearby well-resolved observations to high-redshift observations of partially resolved galaxies. <P />Chapter 4 We present gas-phase metallicity gradients for 94 star-forming galaxies between (0.08 &lt; z &lt; 0.84). We find a negative median metallicity gradient of (-0.043^{+0.009}_{-0.007}, dex/kpc)/span&gt;, i.e. on average we find the centres of these galaxies to be more metal-rich than their outskirts. However, there is significant scatter underlying this and we find that 10% (9) galaxies have significantly positive metallicity gradients, 39% (37) have significantly negative gradients, 28% (26) have gradients consistent with being flat, the remainder 23% (22) are considered to have unreliable gradient estimates. We find a slight trend for a more negative metallicity gradient with both increasing stellar mass and increasing star formation rate (SFR). However, given the potential redshift and size selection effects, we do not consider these trends to be significant. Indeed when we normalize the SFR of our galaxies relative to the main sequence, we do not observe any trend between the metallicity gradient and the normalized SFR. This finding is contrary to other recent studies of galaxies at similar and higher redshifts. We do, however, identify a novel trend between the metallicity gradient of a galaxy and its size. Small galaxies ((r_d &lt; 3 kpc)) present a large spread in observed metallicity gradients (both negative and positive gradients). In contrast, we find no large galaxies (r_d &gt; 3 kpc) with positive metallicity gradients, and overall there is less scatter in the metallicity gradient amongst the large galaxies. We suggest that these large (well-evolved) galaxies may be analogues of galaxies in the present-day Universe, which also present a common negative metallicity gradient. <P />Chapter 5 The relationship between a galaxy's stellar mass and its gas-phase metallicity results from the complex interplay between star formation and the inflow and outflow of gas. Since the gradient of metals in galaxies is also influenced by the same processes, it is therefore natural to contrast the metallicity gradient with the mass-metallicity relation. Here we study the interrelation of the stellar mass, central metallicity and metallicity gradient, using a sample of 72 galaxies spanning (0.13 &lt; z &lt; 0.84) with reliable metallicity gradient estimates. We find that typically the galaxies that fall below the mean mass-metallicity relation have flat or inverted metallicity gradients. We quantify their relationship taking full account of the covariance between the different variables and find that at fixed mass the central metallicity is anti-correlated with the metallicity gradient. We argue that this is consistent with a scenario that suppresses the central metallicity either through the inflow of metal poor gas or outflow of metal enriched gas. <P />\ndoi:10.5281/zenodo.581221\n\n\n"}, {'bibcode': '2017nova.pres.2388K', 'reference': '\n2017nova.pres.2388K\nA 3D View of a Supernova Remnant\nKohler, Susanna\nAAS Nova Highlight, 14 Jun 2017, id.2388\n2017-06-01\nFeatures, Highlights, interstellar medium, stellar evolution, supernova remnant, supernovae, white dwarfs\nhttps://ui.adsabs.harvard.edu/abs/2017nova.pres.2388K\nThe outlined regions mark the 57 knots in Tycho selected by the authors for velocity measurements. Magenta regions have redshifted line-of-sight velocities (moving away from us); cyan regions have blueshifted light-of-sight velocities (moving toward us). [Williams et al. 2017]The Tycho supernova remnant was first observed in the year 1572. Nearly 450 years later, astronomers have now used X-ray observations of Tycho to build the first-ever 3D map of a Type Ia supernova remnant.Signs of ExplosionsSupernova remnants are spectacular structures formed by the ejecta of stellar explosions as they expand outwards into the surrounding interstellar medium.One peculiarity of these remnants is that they often exhibit asymmetries in their appearance and motion. Is this because the ejecta are expanding into a nonuniform interstellar medium? Or was the explosion itself asymmetric? The best way we can explore this question is with detailed observations of the remnants.Histograms of the velocity in distribution of the knots in the X (green), Y (blue) and Z (red) directions (+Z is away from the observer). They show no evidence for asymmetric expansion of the knots. [Williams et al. 2017]Enter TychoTo this end, a team of scientists led by Brian Williams (Space Telescope Science Institute and NASA Goddard SFC) has worked to map out the 3D velocities of the ejecta in the Tycho supernova remnant. Tycho is a Type Ia supernova thought to be caused by the thermonuclear explosion of a white dwarf in a binary system that was destabilized by mass transfer from its companion.After 450 years of expansion, the remnant now has the morphological appearance of a roughly circular cloud of clumpy ejecta. The forward shock wave from the supernova, however, is known to have twice the velocity on one side of the shell as on the other.To better understand this asymmetry, Williams and collaborators selected a total of 57 knots in Tychos ejecta, spread out around the remnant. They then used 12 years of Chandra X-ray observations to measure both the knots proper motion in the plane of the sky and their line-of-sight velocity. These two measurements were then combined to build a full 3D map of the motion of the ejecta.3D hydrodynamical simulations of Tycho, stopped at the current epoch. These show that both initially smooth (top) and initially clumpy (bottom) ejecta models are consistent with the current observations of the morphology and dynamics of Tychos ejecta. [Adapted from Williams et al. 2017]Symmetry and ClumpsWilliams and collaborators found that the knots have total velocities that range from 2400 to 6600 km/s. Unlike the forward shock of the supernova, Tychos ejecta display no asymmetries in their motion which suggests that the explosion itself was symmetric. The more likely explanation is a density gradient in the interstellar medium, which could slow the shock wave on one side of the remnant without yet affecting the motion of the clumps of ejecta.As a final exploration, the authors attempt to address the origin of Tychos clumpiness. The fact that some of Tychos ejecta knots precede its outer edge has raised the question of whether the ejecta started out clumpy, or if they began smooth and only clumped during expansion. Williams and collaborators matched the morphological and dynamical data to simulations, demonstrating that neither scenario can be ruled out at this time.This first 3D map of a Type Ia supernova represents an important step in our ability to understand these stellar explosions. The authors suggest that well be able to expand on this map in the future with additional observations from Chandra, as well as with new data from future X-ray observatories that will be able to detect fainter emission.CitationBrian J. Williams et al 2017 ApJ 842 28. doi:10.3847/1538-4357/aa7384 <P />\n\n\n'}, {'bibcode': '2017CBET.4403....2G', 'reference': '\n2017CBET.4403....2G\nPotential New Meteor Shower from Comet C/2015 D4 (Borisov)\nGreen, D. W. E.\nCentral Bureau Electronic Telegrams, 4403, 2 (2017). Edited by Green, D. W. E.\n2017-06-01\nhttps://ui.adsabs.harvard.edu/abs/2017CBET.4403....2G\nA previous good encounter occurred on 2006 July 29d04h11m UT (r - Delta = +0.0003 AU, solar long. = 125.841 deg). Future encounters are predicted on 2029 July 29d01h53m (+0.0007 AU, 125.816 deg), 2042 July 29d10h48m (+0.0006 AU, 125.886 deg), 2053 July 29d05h35m (+0.0001 AU, 125.848 deg), and on 2068 July 29d02h09m UT (-0.0001 AU, 125.863 deg). <P />\n\n\n'}, {'bibcode': '2017ascl.soft06009C', 'reference': '\n2017ascl.soft06009C\nsick: Spectroscopic inference crank\nCasey, Andrew R.\nAstrophysics Source Code Library, record ascl:1706.009\n2017-06-01\nSoftware\nhttps://ui.adsabs.harvard.edu/abs/2017ascl.soft06009C\nsick infers astrophysical parameters from noisy observed spectra. Phenomena that can alter the data (e.g., redshift, continuum, instrumental broadening, outlier pixels) are modeled and simultaneously inferred with the astrophysical parameters of interest. This package relies on emcee (ascl:1303.002); it is best suited for situations where a grid of model spectra already exists, and one would like to infer model parameters given some data. <P />\n\n\n'}, {'bibcode': '2017yCat.113380453S', 'reference': '\n2017yCat.113380453S\nVizieR Online Data Catalog: BM CVn V-band differential light curve (Siltala+, 2017)\nSiltala, J.\nJetsu, L.\nHackman, T.\nHenry, G. W.\nImmonen, L.\nKajatkari, P.\nLankinen, J.\nLehtinen, J.\nMonira, S.\nNikbakhsh, S.\nViitanen, A.\nViuho, J.\nWillamo, T.\nVizieR On-line Data Catalog: J/AN/338/453. Originally published in: 2017AN....338..453S\n2017-05-01\nStars: variable\nhttps://ui.adsabs.harvard.edu/abs/2017yCat.113380453S\nThe included files present the numerical data of our analysis of the BM CVn photometry. The data consists of differential Johnson V-band photometry using the star HD 116010 as the comparison star. <P />The analysis has been performed using the previously published continuous period search (CPS) method, described in detail in Lehtinen et al., 2011A&amp;A...527A.136L, Cat. J/A+A/527/A136. <P />(4 data files). <P />\n\n\n'}, {'bibcode': '2017AAVSN.429....1W', 'reference': '\n2017AAVSN.429....1W\nV694 Mon (MWC 560) spectroscopy requested\nWaagen, Elizabeth O.\nAAVSO Special Notice #429\n2017-05-01\nastronomical databases: miscellaneous, binaries: symbiotic, stars: individual (V694 Mon, MWC 560)\n(C) AAVSO 2017\nhttps://ui.adsabs.harvard.edu/abs/2017AAVSN.429....1W\nThe observing campaign from 2016 on V694 Mon (MWC 560) (AAVSO Alert Notice 538) has been continued, but with different requirements. Photometry is no longer specifically requested on a regular basis (although ongoing observations that do not interfere with other obligations are welcome). Spectroscopy on a cadence of a week or two is requested to monitor changes in the disk outflow. Investigator Adrian Lucy writes: "Adrian Lucy and Dr. Jeno Sokoloski (Columbia University) have requested spectroscopic monitoring of the broad-absorption-line symbiotic star V694 Mon (MWC 560), as a follow-up to coordinated multi-wavelength observations obtained during its recent outburst (ATel #8653, #8832, #8957; #10281). This system is a perfect place in which to study the relationship between an accretion disk and disk winds/jets, and a high-value target for which even low-resolution spectra can be extraordinarily useful...Optical brightening in MWC 560 tends to predict higher-velocity absorption, but sometimes jumps in absorption velocity also appear during optical quiescence (e.g., Iijima 2001, ASPCS, 242, 187). If such a velocity jump occurs during photometric quiescence, it may prompt radio observations to confirm and test the proposed outflow origin for recently-discovered flat-spectrum radio emission (Lucy et al. ATel #10281)...Furthermore, volunteer spectroscopic monitoring of this system has proved useful in unpredictable ways. For example, \'amateur\' spectra obtained by Somogyi Péter in 2015 December demonstrated that the velocity of absorption was very low only a month before an optical outburst peak prompted absorption troughs up to 3000 km/s, which constrains very well the timing of the changes to the outflow to a degree that would not have been otherwise possible. Any resolution can be useful. A wavelength range that can accommodate a blueshift of at least 140 angstroms (6000 km/s) from the rest wavelengths of H-alpha at 6562 angstroms and/or H-beta at 4861 angstroms is ideal, though spectra with a smaller range can still be useful. Photometry could potentially still be useful, but will be supplementary to medium-cadence photometry being collected by the ANS collaboration." "Spectroscopy may be uploaded to the ARAS database (http://www.astrosurf.com/aras/Aras_DataBase/DataBase.htm), or sent to Adrian and Jeno directly at &lt;lucy@astro.columbia.edu&gt;. Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Photometry should be submitted to the AAVSO International Database. See full Special Notice for more details. <P />\n\n\n'}, {'bibcode': '2017sptz.prop13168Y', 'reference': '\n2017sptz.prop13168Y\nConfirm the Nature of a TDE Candidate in ULIRG F01004-2237 Using Spitzer mid-IR Light Curves\nYan, Lin\nSpitzer Proposal ID 13168\n2017-04-01\nhttps://ui.adsabs.harvard.edu/abs/2017sptz.prop13168Y\nULIRG F01004-2237 had a strong optical flare, peaked in 2010, and the follow-up optical spectra classified this event as a TDE candidate (Tadhunter et al. 2017, Nature Astronomy). In early 2017, using archival WISE data, we discovered that its 3.4 and 4.6um fluxes have been steadily rising since 2013, increased by a factor of 3.5 and 2.6 respectively. The last epoch data from WISE on 2016-12-12 shows that F01004-2237 has reached 7.5 and 14mJy at 3.4 and 4.6um. We interpret the mid-IR LCs as infrared echoes from the earlier optical flare. We infer a convex, dust ring with a radius of 1 pc from the central heating source. Our model predicts that if this event is indeed a TDE, its mid-IR LCs should start to fade in next 5-12 months because it has already reprocessed most of the UV/optical energy from the tidal disruption. However, if this event is due to activities from an AGN, its mid-IR LCs could last over a much longer time scale. We request a total of 3.2 hours of Spitzer time to monitor the mid-IR variations in next 12 months. This will provide the critical data to confirm the nature of this transient event. <P />\n\n\n'}, {'bibcode': '2017MsT..........2A', 'reference': '\n2017MsT..........2A\nSurface Accuracy and Pointing Error Prediction of a 32 m Diameter Class Radio Astronomy Telescope\nAzankpo, Severin\nMasters thesis, University of Stellenbosch, March 2017, 120 pages\n2017-03-01\nhttps://ui.adsabs.harvard.edu/abs/2017MsT..........2A\nThe African Very-long-baseline interferometry Network (AVN) is a joint project between South Africa and eight partner African countries aimed at establishing a VLBI (Very-Long-Baseline Interferometry) capable network of radio telescopes across the African continent. An existing structure that is earmarked for this project, is a 32 m diameter antenna located in Ghana that has become obsolete due to advances in telecommunication. The first phase of the conversion of this Ghana antenna into a radio astronomy telescope is to upgrade the antenna to observe at 5 GHz to 6.7 GHz frequency and then later to 18 GHz within a required performing tolerance. The surface and pointing accuracies for a radio telescope are much more stringent than that of a telecommunication antenna. The mechanical pointing accuracy of such telescopes is influenced by factors such as mechanical alignment, structural deformation, and servo drive train errors. The current research investigates the numerical simulation of the surface and pointing accuracies of the Ghana 32 m diameter radio astronomy telescope due to its structural deformation mainly influenced by gravity, wind and thermal loads. <P />\n\n\n'}, {'bibcode': '2016emo6.rept.....R', 'reference': "\n2016emo6.rept.....R\nThe penumbral Moon's eclipse form 16 september 2016\nRotaru, Adrian\nPteancu, Mircea\nZaharia, Cristian\nhttp://www.astronomy.ro/forum/viewtopic.php?p=159287#159287 (Comments in Romanian)\n2016-10-01\nTHE MOON, ECLIPSES, PARTIAL, PENUMBRAL, ASTROPHOTOGRAPHY\nhttps://ui.adsabs.harvard.edu/abs/2016emo6.rept.....R\nThe web page represents circumstances and photographs from the Moon's partial/penumbral eclipse from 16 September 2016 obtained from few various places in Romania (East Europe). A part of photographs give the maximum phase of the Eclipse, while another give the reddened Moon. <P />\n\n\n"}, {'bibcode': '2016iac..talk..872V', 'reference': '\n2016iac..talk..872V\nLiving on the edge: Adaptive Optics+Lucky Imaging\nVelasco, Sergio\nIAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrofísica de Canarias, 872\n2016-03-01\nhttps://ui.adsabs.harvard.edu/abs/2016iac..talk..872V\nNot Available <P />\n\n\n'}, {'bibcode': '2009bcet.book...65L', 'reference': '\n2009bcet.book...65L\nThe Diversity of Nuclear Magnetic Resonance Spectroscopy\nLiu, Corey W.\nAlekseyev, Viktor Y.\nAllwardt, Jeffrey R.\nBankovich, Alexander J.\nCade-Menun, Barbara J.\nDavis, Ronald W.\nDu, Lin-Shu\nGarcia, K. Christopher\nHerschlag, Daniel\nKhosla, Chaitan\nKraut, Daniel A.\nLi, Qing\nNull, Brian\nPuglisi, Joseph D.\nSigala, Paul A.\nStebbins, Jonathan F.\nVarani, Luca\nBiophysics and the Challenges of Emerging Threats, NATO Science for Peace and Security Series B: Physics and Biophysics. ISBN 978-90-481-2367-4. Springer Netherlands, 2009, p. 65\n2009-01-01\nPhysics\n(c) 2009: Springer Netherlands\nhttps://ui.adsabs.harvard.edu/abs/2009bcet.book...65L\nThe discovery of the physical phenomenon of Nuclear Magnetic Resonance (NMR) in 1946 gave rise to the spectroscopic technique that has become a remarkably versatile research tool. One could oversimplify NMR spectros-copy by categorizing it into the two broad applications of structure elucidation of molecules (associated with chemistry and biology) and imaging (associated with medicine). But, this certainly does not do NMR spectroscopy justice in demonstrating its general acceptance and utilization across the sciences. This manuscript is not an effort to present an exhaustive, or even partial review of NMR spectroscopy applications, but rather to provide a glimpse at the wide-ranging uses of NMR spectroscopy found within the confines of a single magnetic resonance research facility, the Stanford Magnetic Resonance Laboratory. Included here are summaries of projects involving protein structure determination, mapping of intermolecular interactions, exploring fundamental biological mechanisms, following compound cycling in the environmental, analysis of synthetic solid compounds, and microimaging of a model organism. <P />\ndoi:10.1007/978-90-481-2368-1_5\n\n\n'}, {'bibcode': '2007AAS...210.2104M', 'reference': '\n2007AAS...210.2104M\nTime Domain Exploration with the Palomar-QUEST Sky Survey\nMahabal, Ashish A.\nDrake, A. J.\nDjorgovski, S. G.\nDonalek, C.\nGlikman, E.\nGraham, M. J.\nWilliams, R.\nBaltay, C.\nRabinowitz, D.\nPQ Team Caltech\nYale\nNCSA\nIndiana\n, . . .\nAmerican Astronomical Society Meeting 210, id.21.04\n2007-05-01\nhttps://ui.adsabs.harvard.edu/abs/2007AAS...210.2104M\nPalomar-QUEST (PQ) synoptic sky survey has now been routinely processing data from driftscans in real-time. As four photometric bandpasses are utilized in nearly simultaneously, PQ is well suited to search for transient and highly variable objects. Using a series of software filters i.e. programs to select/deselect objects based on certain criteria we shorten the list of candidates from the initially flagged candidate transients. Such filters include looking for known asteroids, known variables, as well as moving, but previously uncatalogued objects based on their motion within a scan as well as between successive scans. Some software filters also deal with instrumental artifacts, edge effects, and use clustering of spurious detections around bright stars. During a typical night when we cover about 500 sq. degrees, we detect hundreds of asteroids, the primary contaminants in the search for astrophysical transients beyond our solar system. <P />Here we describe some statistics based on the software filters we employ and the nature of the objects that seem to survive the process. We also discuss the usefulness of this to amateur astronomers, projects like VOEventNet, and other synoptic sky surveys. <P />We also present an outline of the work we have started on quantifying the variability of quasars, blazars, as well as various classes of Galactic sources, by combining the large number of PQ scans with other existing data sources federated in the Virtual Observatory environment. <P />The PQ survey is partially supported by the U.S. National Science Foundation (NSF). <P />\n\n\n'}, {'bibcode': '2007RJPh....1...35.', 'reference': '\n2007RJPh....1...35.\nAnalysis of Thermal Losses in the Flat-Plate Collector of a Thermosyphon Solar Water Heater\n., S. N. Agbo\n., E. C. Okoroigwe\nResearch Journal of Physics, vol. 1, issue 1, pp. 35-41\n2007-01-01\nhttps://ui.adsabs.harvard.edu/abs/2007RJPh....1...35.\nNot Available <P />\ndoi:10.3923/rjp.2007.35.41\n\n\n'}, {'bibcode': '1995ans..agar..390M', 'reference': '\n1995ans..agar..390M\nSpacecraft navigation requirements\nMiller, Judy L.\nIn AGARD, Aerospace Navigation Systems p 390-405 (SEE N96-13404 02-04)\n1995-06-01\nEarth Orbits, Navigation Aids, Navigators, Onboard Equipment, Space Navigation, Spacecraft Trajectories, Support Systems, Technology Assessment, Technology Utilization, Ascent Trajectories, Reentry Trajectories, Spacecraft, Spacecraft Performance, Spacecraft Survivability, Tradeoffs, Weight (Mass), Space Communications, Spacecraft Communications, Command and Tracking\nhttps://ui.adsabs.harvard.edu/abs/1995ans..agar..390M\nSpacecraft operation depends upon knowledge of vehicular position and, consequently, navigational support has been required for all such systems. Technical requirements for different mission trajectories and orbits are addressed with consideration given to the various tradeoffs which may need to be considered. The broad spectrum of spacecraft are considered with emphasis upon those of greater military significance (i.e., near earth orbiting satellites). Technical requirements include, but are not limited to, accuracy; physical characteristics such as weight and volume; support requirements such as electrical power and ground support; and system integrity. Generic navigation suites for spacecraft applications are described. It is shown that operational spacecraft rely primarily upon ground-based tracking and computational centers with little or no navigational function allocated to the vehicle, while technology development efforts have been and continue to be directed primarily toward onboard navigation suites. The military significance of onboard navigators is shown to both improve spacecraft survivability and performance (accuracy). <P />\n\n\n'}, {'bibcode': '1995anda.book.....N', 'reference': '\n1995anda.book.....N\nApplied nonlinear dynamics: analytical, computational and experimental methods\nNayfeh, Ali H.\nBalachandran, Balakumar\nWiley series in nonlinear science, New York; Chichester: Wiley, |c1995\n1995-01-01\nhttps://ui.adsabs.harvard.edu/abs/1995anda.book.....N\ncitations:118\nNot Available <P />\n\n\n'}, {'bibcode': '1991hep.th....8028G', 'reference': '\n1991hep.th....8028G\nApplied Conformal Field Theory\nGinsparg, Paul\neprint arXiv:hep-th/9108028\n1988-11-01\nHigh Energy Physics - Theory\nhttps://ui.adsabs.harvard.edu/abs/1991hep.th....8028G\ncitations:190\nThese lectures consisted of an elementary introduction to conformal field theory, with some applications to statistical mechanical systems, and fewer to string theory. Contents: 1. Conformal theories in d dimensions 2. Conformal theories in 2 dimensions 3. The central charge and the Virasoro algebra 4. Kac determinant and unitarity 5. Identication of m = 3 with the critical Ising model 6. Free bosons and fermions 7. Free fermions on a torus 8. Free bosons on a torus 9. Affine Kac-Moody algebras and coset constructions 10. Advanced applications <P />\n\n\n'}, {'bibcode': '1983aiaa.meetY....K', 'reference': "\n1983aiaa.meetY....K\nAutonomous navigation using lunar beacons\nKhatib, A. R.\nEllis, J.\nFrench, J.\nNull, G.\nYunck, T.\nWu, S.\nAmerican Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 21st, Reno, NV, Jan. 10-13, 1983. 7 p.\n1983-01-01\nArtificial Satellites, Autonomous Navigation, Earth-Moon System, Lunar Communication, Radio Beacons, Radio Navigation, Space Navigation, Doppler Navigation, Least Squares Method, Orbit Calculation, Space Communications, Spacecraft Communications, Command and Tracking\nhttps://ui.adsabs.harvard.edu/abs/1983aiaa.meetY....K\nThe concept of using lunar beacon signal transmission for on-board navigation for earth satellites and near-earth spacecraft is described. The system would require powerful transmitters on the earth-side of the moon's surface and black box receivers with antennae and microprocessors placed on board spacecraft for autonomous navigation. Spacecraft navigation requires three position and three velocity elements to establish location coordinates. Two beacons could be soft-landed on the lunar surface at the limits of allowable separation and each would transmit a wide-beam signal with cones reaching GEO heights and be strong enough to be received by small antennae in near-earth orbit. The black box processor would perform on-board computation with one-way Doppler/range data and dynamical models. Alternatively, GEO satellites such as the GPS or TDRSS spacecraft can be used with interferometric techniques to provide decimeter-level accuracy for aircraft navigation. <P />\n\n\n"}, {'bibcode': '2012ddsw.rept.....T', 'reference': '\n2012ddsw.rept.....T\nDaymet: Daily surface weather on a 1 km grid for North America, 1980-2008\nThornton, P. E.\nThornton, M. M.\nMayer, B. W.\nWilhelmi, N.\nWei, Y.\nDevarakonda, R.\nCook, R.\nOak Ridge National Laboratory (ORNL) Distributed Active Archive Center for Biogeochemical Dynamics (DAAC)\n2012-04-01\nDaymet\nOak Ridge National Laboratory\nhttps://ui.adsabs.harvard.edu/abs/2012ddsw.rept.....T\ncitations:51\nArchived and distributed through the ORNL DAAC, the Daymet data set provides gridded estimates of daily weather parameters for North America, including daily continuous surfaces of minimum and maximum temperature, precipitation occurrence and amount, humidity, shortwave radiation, snow water equivalent, and day length. The daily time step, 1 km x 1 km spatial resolution, and North American spatial extent of the data set makes it a unique and valuable contribution to scientific, research, and educational communities. The literature shows that Daymet data have been broadly applied to fields including hydrology, terrestrial vegetation growth models, carbon cycle science, and regional to large scale climate change analysis.\ndoi:10.3334/ORNLDAAC/1219\n\n\n'}, {'bibcode': '2020EPJC...80...96D', 'reference': '\n2020EPJC...80...96D\nGeneralized Lomb–Scargle analysis of 36Cl decay rate measurements at PTB and BNL\nDhaygude, Akanksha\nDesai, Shantanu\nThe European Physical Journal C, Volume 80, Issue 2, article id.96\n2020-02-01\nAstrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Nuclear Experiment\n© The Author(s) 2020\nhttps://ui.adsabs.harvard.edu/abs/2020EPJC...80...96D\nRecently Pomme et al. (Solar Phys 292:162, 2017) did an analysis of 36Cl radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookhaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2 to 20/year. We carry out an independent analysis of the same PTB and BNL data, using the generalized Lomb–Scargle periodogram to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al., but the significance is much lower. All our analysis codes and datasets have been made publicly available.\ndoi:10.1140/epjc/s10052-020-7683-6; 10.48550/arXiv.1912.06970\n\n\n'}], 'header': '\n\n', 'footer': ''} diff --git a/exportsrv/tests/unittests/test_export_service.py b/exportsrv/tests/unittests/test_export_service.py index a7aa6c2..df621b6 100755 --- a/exportsrv/tests/unittests/test_export_service.py +++ b/exportsrv/tests/unittests/test_export_service.py @@ -948,6 +948,10 @@ def test_encode_laTex(self): expected2 = "This is a $ math mode $ example." self.assertEqual(encode_laTex(text2), expected2) + # text with mathML markup + text3 = "Generalized Lomb-Scargle analysis of 36Cl decay rate measurements at PTB and BNL" + expected3 = "Generalized Lomb-Scargle analysis of 36Cl decay rate measurements at PTB and BNL" + self.assertEqual(encode_laTex(text3), expected3) def test_utf8tolatex(self): """ test the main loop of utf8tolatex function to ensure correct processing of ASCII and non-ASCII characters """ diff --git a/exportsrv/tests/unittests/test_solrdata.py b/exportsrv/tests/unittests/test_solrdata.py index 165f545..cf9dced 100644 --- a/exportsrv/tests/unittests/test_solrdata.py +++ b/exportsrv/tests/unittests/test_solrdata.py @@ -38,7 +38,7 @@ def test_get_solr_data(self): matched += 1 self.assertEqual(matched, len(bibcodes)) - # the mock is for solr call bigquery, with 23 bibcodes + # the mock is for solr call bigquery, with 24 bibcodes with mock.patch.object(self.current_app.client, 'post') as post_mock: post_mock.return_value = mock_response = mock.Mock() mock_response.json.return_value = solrdata.data @@ -48,7 +48,7 @@ def test_get_solr_data(self): "2017ascl.soft06009C", "2017yCat.113380453S", "2017AAVSN.429....1W", "2017sptz.prop13168Y", "2017MsT..........2A", "2016emo6.rept.....R", "2016iac..talk..872V", "2009bcet.book...65L", "2007AAS...210.2104M", "2007RJPh....1...35.", "1995ans..agar..390M", "1995anda.book.....N", - "1991hep.th....8028G", "1983aiaa.meetY....K", "2012ddsw.rept.....T"] + "1991hep.th....8028G", "1983aiaa.meetY....K", "2012ddsw.rept.....T", "2020EPJC...80...96D"] solr_data = get_solr_data(bibcodes=bibcodes, fields='bibcode,author,year,pub,bibstem', sort='') matched = 0 diff --git a/exportsrv/utils.py b/exportsrv/utils.py index 5d8f467..e4f1eae 100644 --- a/exportsrv/utils.py +++ b/exportsrv/utils.py @@ -7,6 +7,7 @@ from flask import current_app, request import requests import re +from lxml import etree from exportsrv.formatter.ads import adsFormatter @@ -162,3 +163,33 @@ def replace_html_entity(text, encode_style): text = re.sub(entity, html_entity_to_encode.get(entity, ''), text) return text + +def mathml_to_plaintext(text): + REGEX_MATHML = re.compile(r"", re.DOTALL) + def replace_mathml(match): + chunk = match.group(0) + + # Insert namespace so mml: tags are parsed properly + cleaned = ( + chunk + .replace("", "") + .replace("``", "\"") + .replace("''", "\"") + ) + + parser = etree.XMLParser(recover=True) + try: + root = etree.fromstring(cleaned.encode(), parser=parser) + if root is None: + return "" + # Find the element + math_el = root.xpath(".//*[local-name()='math']") + if math_el: + # Extract all text inside + return "".join(math_el[0].itertext()).strip() + except Exception as e: + return "" + return "" + + return REGEX_MATHML.sub(replace_mathml, text) From 720da766fe5f2186ddccffbdf62b8b516614cc97 Mon Sep 17 00:00:00 2001 From: Kelly Lockhart <2926089+kelockhart@users.noreply.github.com> Date: Thu, 3 Jul 2025 16:37:40 -0400 Subject: [PATCH 2/3] Refactored --- exportsrv/formatter/toLaTex.py | 56 +--------------------------------- exportsrv/utils.py | 54 ++++++++++++++++++++++++++++++++ 2 files changed, 55 insertions(+), 55 deletions(-) diff --git a/exportsrv/formatter/toLaTex.py b/exportsrv/formatter/toLaTex.py index 4c6d255..3fd22ab 100755 --- a/exportsrv/formatter/toLaTex.py +++ b/exportsrv/formatter/toLaTex.py @@ -3,7 +3,7 @@ import re from collections import OrderedDict from exportsrv.formatter.latexencode import utf8tolatex -from lxml import etree +from exportsrv.utils import mathml_to_latex # this module contains methods to encode for latex output @@ -119,57 +119,3 @@ def html_to_laTex(text): text = key.sub(REGEX_HTML_TAG[key], text) return text - -def convert_mathml_element(el): - if not isinstance(el, etree._Element): - return "" - - tag = etree.QName(el).localname - - if tag == "msup": - base = convert_mathml_element(el[0]).strip() or "{}" - exp = convert_mathml_element(el[1]).strip() - return f"{base}$^{{{exp}}}$" - - if tag == "msub": - base = convert_mathml_element(el[0]).strip() or "{}" - sub = convert_mathml_element(el[1]).strip() - return f"{base}$_{{{sub}}}$" - - if tag == "mn" or tag == "mi": - return "".join(el.itertext()).strip() - - if tag == "mrow": - return "".join([convert_mathml_element(child) for child in el]) - - # fallback - return "".join(el.itertext()).strip() - -def mathml_to_latex(text): - # Regex to find ... blocks - pattern = re.compile(r"", re.DOTALL) - - def replace_mathml(match): - chunk = match.group(0) - # Clean the chunk so it's parseable - cleaned = ( - chunk - # have to squish the mathML markup into an XML format for lxml to work - .replace("", "") - .replace("``", "\"").replace("''", "\"") - ) - - parser = etree.XMLParser(recover=True) - try: - root = etree.fromstring(cleaned.encode(), parser=parser) - mml_math = root.xpath(".//*[local-name()='math']") # this will return an array - if mml_math: - return convert_mathml_element(mml_math[0]) - else: - return "[MATHML]" - except Exception as e: - return "[MATHML_ERROR]" - - # Substitute all MathML chunks with LaTeX equivalents - return pattern.sub(replace_mathml, text) diff --git a/exportsrv/utils.py b/exportsrv/utils.py index e4f1eae..e0fb016 100644 --- a/exportsrv/utils.py +++ b/exportsrv/utils.py @@ -193,3 +193,57 @@ def replace_mathml(match): return "" return REGEX_MATHML.sub(replace_mathml, text) + +def mathml_to_latex(text): + # Regex to find ... blocks + pattern = re.compile(r"", re.DOTALL) + + def convert_mathml_element(el): + if not isinstance(el, etree._Element): + return "" + + tag = etree.QName(el).localname + + if tag == "msup": + base = convert_mathml_element(el[0]).strip() or "{}" + exp = convert_mathml_element(el[1]).strip() + return f"{base}$^{{{exp}}}$" + + if tag == "msub": + base = convert_mathml_element(el[0]).strip() or "{}" + sub = convert_mathml_element(el[1]).strip() + return f"{base}$_{{{sub}}}$" + + if tag == "mn" or tag == "mi": + return "".join(el.itertext()).strip() + + if tag == "mrow": + return "".join([convert_mathml_element(child) for child in el]) + + # fallback + return "".join(el.itertext()).strip() + + def replace_mathml(match): + chunk = match.group(0) + # Clean the chunk so it's parseable + cleaned = ( + chunk + # have to squish the mathML markup into an XML format for lxml to work + .replace("", "") + .replace("``", "\"").replace("''", "\"") + ) + + parser = etree.XMLParser(recover=True) + try: + root = etree.fromstring(cleaned.encode(), parser=parser) + mml_math = root.xpath(".//*[local-name()='math']") # this will return an array + if mml_math: + return convert_mathml_element(mml_math[0]) + else: + return "[MATHML]" + except Exception as e: + return "[MATHML_ERROR]" + + # Substitute all MathML chunks with LaTeX equivalents + return pattern.sub(replace_mathml, text) From bcfa8ba1be9a26063005384aedd95f51b60c9e14 Mon Sep 17 00:00:00 2001 From: Kelly Lockhart <2926089+kelockhart@users.noreply.github.com> Date: Thu, 3 Jul 2025 16:54:20 -0400 Subject: [PATCH 3/3] Refactoring part 2 --- exportsrv/utils.py | 91 +++++++++++++++++++++------------------------- 1 file changed, 41 insertions(+), 50 deletions(-) diff --git a/exportsrv/utils.py b/exportsrv/utils.py index e0fb016..abc9ef4 100644 --- a/exportsrv/utils.py +++ b/exportsrv/utils.py @@ -164,12 +164,15 @@ def replace_html_entity(text, encode_style): return text -def mathml_to_plaintext(text): +def process_mathml(text, converter_func): + """ + Generic processor: Replaces all MathML inline formulas + using the provided converter_func. + """ REGEX_MATHML = re.compile(r"", re.DOTALL) def replace_mathml(match): chunk = match.group(0) - # Insert namespace so mml: tags are parsed properly cleaned = ( chunk .replace(" element math_el = root.xpath(".//*[local-name()='math']") if math_el: - # Extract all text inside - return "".join(math_el[0].itertext()).strip() - except Exception as e: + return converter_func(math_el[0]) + except Exception: return "" return "" return REGEX_MATHML.sub(replace_mathml, text) -def mathml_to_latex(text): - # Regex to find ... blocks - pattern = re.compile(r"", re.DOTALL) +def convert_to_plaintext(el): + """ + Simply concatenates all text content inside the MathML element. + """ + return "".join(el.itertext()).strip() - def convert_mathml_element(el): - if not isinstance(el, etree._Element): - return "" +def convert_to_latex(el): + """ + Recursively converts MathML elements into LaTeX. + """ + if not isinstance(el, etree._Element): + return "" - tag = etree.QName(el).localname + # Safer tag handling + if el.tag.startswith("{"): + tag = el.tag.split("}", 1)[1] + else: + tag = el.tag - if tag == "msup": - base = convert_mathml_element(el[0]).strip() or "{}" - exp = convert_mathml_element(el[1]).strip() - return f"{base}$^{{{exp}}}$" + if tag == "msup": + base = convert_to_latex(el[0]).strip() or "{}" + exp = convert_to_latex(el[1]).strip() + return f"{base}$^{{{exp}}}$" - if tag == "msub": - base = convert_mathml_element(el[0]).strip() or "{}" - sub = convert_mathml_element(el[1]).strip() - return f"{base}$_{{{sub}}}$" + if tag == "msub": + base = convert_to_latex(el[0]).strip() or "{}" + sub = convert_to_latex(el[1]).strip() + return f"{base}$_{{{sub}}}$" - if tag == "mn" or tag == "mi": - return "".join(el.itertext()).strip() + if tag in ("mn", "mi", "mtext"): + return "".join(el.itertext()).strip() - if tag == "mrow": - return "".join([convert_mathml_element(child) for child in el]) + if tag == "mrow": + return "".join([convert_to_latex(child) for child in el]) - # fallback - return "".join(el.itertext()).strip() + # Fallback + return "".join(el.itertext()).strip() - def replace_mathml(match): - chunk = match.group(0) - # Clean the chunk so it's parseable - cleaned = ( - chunk - # have to squish the mathML markup into an XML format for lxml to work - .replace("", "") - .replace("``", "\"").replace("''", "\"") - ) +def mathml_to_plaintext(text): + return process_mathml(text, convert_to_plaintext) - parser = etree.XMLParser(recover=True) - try: - root = etree.fromstring(cleaned.encode(), parser=parser) - mml_math = root.xpath(".//*[local-name()='math']") # this will return an array - if mml_math: - return convert_mathml_element(mml_math[0]) - else: - return "[MATHML]" - except Exception as e: - return "[MATHML_ERROR]" - - # Substitute all MathML chunks with LaTeX equivalents - return pattern.sub(replace_mathml, text) +def mathml_to_latex(text): + return process_mathml(text, convert_to_latex)