adsabs/WIESP2022-NER huggingface dataset:
Paper: 2016MNRAS.457.3448I (acknowledgments)
The scientific results reported in this article are based on observations obtained with the Chandra X-ray Observatory and XMM–Newton , an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package ciao , and of softwares and tools provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research is based on observations with the NASA/UK/ASI Swift mission. We thank N. Schartel for approving the XMM–Newton 2014 November observation through the Director's Discretionary Time program and the staff of the XMM–Newton Science Operation Center for performing the Target of Opportunity observations. Similarly, we thank B. Wilkes for approving the Chandra 2014 August observation through the Director's Discretionary Time program and the Chandra staff for performing the Target of Opportunity observations. We thank the Swift duty scientists and science planners for making these observations possible. The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The authors warmly thank Phil Edwards for the prompt scheduling of the observations and John Reynolds for releasing part of the telescope time of his project. We thanks Jules Halpern for useful comments. NR is supported by an NWO Vidi Grant, and by grants AYA2012-39303 and SGR2014-1073. This work is partially supported by the European COST Action MP1304 (NewCOMPSTAR).
Paper: 2018MNRAS.476..366B (acknowledgments)
Acknowledgements TB acknowledges support from Fundação para a Ciência e a Tecnologia (grant SFRH/BPD/122325/2016), and support from Center for Research Development in Mathematics and Applications (CIDMA) (strategic project UID/MAT/04106/2013), and from ENGAGE SKA, POCI-01-0145-FEDER-022217, funded by COMPETE 2020 and FCT, Portugal. DRGS and BR thank for funding through Fondecyt regular (project code 1161247). BR thanks Conicyt for financial support (CONICYT-PFCHA/MagísterNacional/2017-22171385). DRGS, MF, and AMS acknowledge funding through the ‘Concurso Proyectos Internacionales de Investigación, Convocatoria 2015’ (project code PII20150171) and the BASAL Centro de Astrofísica y Tecnologías Afines (CATA) PFB-06/2007. DRGS is further grateful for funding via ALMA-Conicyt (project code 31160001), Quimal (project code QUIMAL170001), and the Anillo program ‘Formation and Growth of Supermassive Black Holes’ (project code ACT172033). RSK acknowledges financial support from the Deutsche Forschungsgemeinschaft via SFB 881 ‘The Milky Way System’ (sub-projects B1, B2, and B8) and SPP 1573 ‘Physics of the Interstellar Medium’. LH and RSK were supported by the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007–2013) via the ERC Advanced Grant ‘STARLIGHT: Formation of the First Stars’ (project number 339177).
Paper: 2018ApJ...852..140W (acknowledgments)
We are grateful to Stephen Justham at National Astronomical Observatories, Chinese Academy of Sciences (CAS), for discussions. R.X.X. acknowledges the support of National Key RD Program of China (No. 2017YFA0402602), National Natural Science Foundation of China (NSFC) 11673002 and U1531243. W.Y.W. and X.L.C. acknowledge the support of MoST 2016YFE0100300, NSFC 11473044, 11633004, 11373030, CAS QYZDJ-SSW-SLH017. R.L. and K.J.L. are supported by NSFC U15311243 National Basic Research Program of China, 973 Program, 2015CB857101, XDB23010200, 11690024, 11373011, and funding from the Max-Planck Partner Group.
Paper: 2016ApJ...824...15V (acknowledgments)
We thank Kevin Schlaufman, Saul Rappaport, Jens Jessen-Hansen, and the anonymous referee for helpful comments and suggestions that have significantly improved this manuscript. Part of this manuscript was written at MIT and V.V.E. appreciates the hospitality of the researchers and staff at the MIT Kavli Institute for Astrophysics and Space Research. Work by J..N.W. was partly supported by funding from the NASA Origins program (grant ID NNX11AG85G). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No. DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler ) funded by the European Research Council (grant agreement No. 267864). We acknowledge ASK for covering travels in relation to this publication. Part of this work was supported by the Danish Council for Independent Research, through a DFF Sapere Aude Starting grant No. 4181-00487B.
Paper: 2016MNRAS.460L..15M (acknowledgments)
The authors thank J. Zibin for his useful comments on the letter. Partial financial support from the Spanish Ministerio de Economía y Competitividad Projects AYA2012-39475-C02-01 and Consolider-Ingenio 2010 CSD2010-00064 is acknowledged.
Paper: 2015MNRAS.450..160B (acknowledgments)
We thank the authors of the atlas9 , marcs , phoenix and drift-phoenix model atmosphere grids to allow us to use their model results for this comparison study, and for their helpful suggestions. We thank Dr Tim-Oliver Husser (Institut für Astrophysik, Georg-August-Universitat Göttingen) for his support with the phoenix models. We also thank Sören Witte and our referee for constructive feedback. ChH highlights financial support of the European Community under the FP7 by an ERC starting grant. IB thanks the Physics Trust of the University of St Andrews for supporting her summer placement. Most literature search was performed using the ADS. Our local computer support is highly acknowledged.
Paper: 2018ApJ...864..113R (acknowledgments)
The authors thank the anonymous referee for constructive comments on the manuscript. The numerical simulations were performed on facilities hosted by the CSC-IT Center for Science in Espoo, Finland. A.R. acknowledges support from the MPA Garching Visitor Programme. A.R. is funded by the doctoral program of Particle Physics and Universe Sciences at the University of Helsinki. P.H.J. and A.R. acknowledge the support of Academy of Finland grant 274931. T.N. acknowledges support from the DFG Cluster of Excellence “Origin and Structure of the Universe.”
Paper: 2016MNRAS.463..393L (acknowledgments)
The authors would like to thank Scott Tremaine for helpful discussions.
Paper: 2018MNRAS.481.4621Q (acknowledgments)
ACKNOWLEDGEMENTS This work is supported by the Natural Sciences and Engineering Research Council of Canada through a Discovery Accelerator Supplement under Grant RGPAS-493042-2016.
Paper: 2019MNRAS.485.2083W (acknowledgments)
ACKNOWLEDGEMENTS We thank Volker Springel for helpful comments, and Dylan Nelson for providing videos of the merging histories of galaxies in Illustris to help us understand the processes better. LW acknowledges support from the National Natural Science Foundation of China grants program (No.11573031), and the National Key Program for Science and Technology Research and Development (2017YFB0203300). QG is supported by two National Natural Science Foundation of China grants (Nos 11573033 and 11622325).
Paper: 2018ApJ...854...20B (acknowledgments)
D. Berdichevsky provided support in the difficult and lengthy process of calibrating the data. N.F.N. and L.F.B. were supported by the NASA Voyager Project under a cooperative agreement to the University of Maryland, Baltimore County. V.F. was supported by NASA grants NNX113AF99G and NNX17AB85G. He also acknowledges support from the International Space Science Institute in Bern in the framework of the team “The Physics of the Very Local Interstellar Medium.”
Paper: 2019A&A...628A..88B (acknowledgments)
Acknowledgements This work was supported by the Labex P2IO project A-JWST-01-02-01+LABEXP2IOPDO and the Programme National de Physique Stellaire (PNPS) of CNRS/INSU co-funded by CEA and CNES. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in Ochsenbein et al. (2000) .
Paper: 2018MNRAS.473.2304P (acknowledgments)
Acknowledgements The authors wish to thank Jan-Uwe Ness, Karl Foster, Ignacio de la Calle and the rest of the XMM-Newton and NuSTAR scheduling teams for the support that made the coordinated observations possible. We would like to thank the referee for the helpful comments and careful reading of the paper. The GC XMM-Newton monitoring project is supported by the Bundesministerium für Wirtschaft und Technologie/Deutsches Zentrum für Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408 and FKZ 50 OR 1408) and the Max Planck Society. SB acknowledges financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0. TMD acknowledges support via a Ramón y Cajal Fellowship (RYC-2015-18148). BDM acknowledges support from the European Union's Horizon 2020 research and innovation programme and the Polish National Science Centre grant Polonez 2016/21/P/ST9/04025. These results are based on observations obtained with XMM-Newton , an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the nustardas jointly developed by the ASI Science Data Centre (ASDC, Italy) and the California Institute of Technology (USA). We thank the staff of the GMRT who have made these observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1).
Paper: 2015MNRAS.454.4182C (acknowledgments)
The author is supported by the Royal Society as a Royal Society University Research Fellow at the University of Cambridge, UK.
Paper: 2018MNRAS.476.3097L (acknowledgments)
ACKNOWLEDGEMENTS We are grateful for a careful reading of our paper and many helpful comments from an anonymous referee. The authors would like to thank Jay Lockman, Andrew Robinson, and Jeyhan Kartaltepe for helpful discussions. AL is supported by the National Radio Astronomy Observatory under the Student Observing Support program project GBT 16B-285. SC acknowledges support from National Science Foundation grant number 1517488. YS is partially supported by the National Natural Science Foundation of China (NSFC) grant 11603032. The authors would like to thank the Sloan Digital Sky Survey for making all their data public and easily accessible and Barbara Catinella and the GASS collaboration for making their data public. The National Radio Astronomy Observatory and the Green Bank Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non- HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.
Paper: 2020A&A...634A..63K (acknowledgments)
We sincerely thank Dr. Clara Froment for her constructive comments that improved the paper significantly. We would like to thank Dr. Bart De Pontieu (LMSAL) for helpful comments on a previous version of the paper. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. S.K.T. gratefully acknowledges support by the NASA contract NNG09FA40C (IRIS). AKS and MM acknowledge the support of the UGC-UKIERI grant to support the present research.
Paper: 2016MNRAS.455..476S (acknowledgments)
We thank Yehuda Hoffman for making the CLUES initial conditions available. IMS-S, CBB and GY thank the MINECO (Spain) for the financial support through the AYA2012-31101 grant. CBB is funded through the Ramon y Cajal programme of the MINECO. The CLUES simulations were performed and analysed at the High Performance Computing Center Stuttgart (HLRS). We thank DEISA for access to computing resources through DECI projects SIMU-LU and SIMUGAL-LU and the generous allocation of resources from STFC's DiRAC Facility (COSMOS: Galactic Archaeology), the DEISA consortium, co-funded through EU FP6 project RI-031513 and the FP7 project RI-222919 (through the DEISA Extreme Computing Initiative), the PRACE-2IP Project (FP7 RI-283493).
Paper: 2016ApJ...823...46F (acknowledgments)
We thank Bill Paxton, Josiah Schwab, Pablo Marchant, Rich Townsend, Matteo Cantiello, and Lars Bildsten for engaging conversations about the MESA project. We also thank Michael Wiescher for initial discussions about this paper. This project was supported by NASA under the Theoretical and Computational Astrophysics Networks grant NNX14AB53G and the Astrophysics Theory Program grant 14-ATP14-0007, and by NSF under the Software Infrastructure for Sustained Innovation grant 1339600, and grant PHY 08-022648 for the Physics Frontier Center “Joint Institute for Nuclear Astrophysics—Center for the Evolution of the Elements” (JINA-CEE). C.E.F. acknowledges support from Arizona State University under a 2015 CLAS Undergraduate Summer Enrichment Award, a 2015-2016 Norm Perrill Origins Project Undergraduate Scholarship, and a ASU/NASA Space Grant award. F.X.T. acknowledges sabbatical support from the Simons Foundation.
Paper: 2019A&A...622A.169M (acknowledgments)
The authors acknowledge the contribution of the FP7 SPACE project ASTRODEEP (Ref. No: 312725), supported by the European Commission. We thank the anonymous referee for the useful comments and suggestions that greatly helped us to improve the paper.
Paper: 2017A&A...601A.133R (acknowledgments)
The Liège team acknowledges support from the Fonds de la Recherche Scientifique (F.R.S/FNRS) including especially an F.R.S/FNRS Research Project (T.0100.15), as well as through an ARC grant for Concerted Research Actions financed by the French Community of Belgium (Wallonia-Brussels Federation), and an XMM PRODEX contract (Belspo). We are particularly grateful to Reinhold Haefner for having made his IBVS data available and to Ella Antokhina and Igor Antokhin for discussions on the photometric solution. EG is greatly indebted to Stephanie Wachter and Suzanne Tourtelotte for having spared no pains in facilitating the interaction with the YALO archives. We are grateful to I. Stevens, H. Sana, Y. Nazé, J.-M. Vreux, and M. da Silva Pires for taking some of the spectroscopic data or for discussions on earlier versions of this work. We thank John Hillier for making his code available.
Paper: 2019MNRAS.484..125R (acknowledgments)
ACKNOWLEDGEMENTS DLL thanks the Robert A. Welch Foundation of Houston, Texas for support through grant F-634. We thank the referee for a constructive report.
Paper: 2019ApJ...872...77S (acknowledgments)
K.S.R. acknowledges the financial support from the Science Engineering Research Board (SERB), Department of Science Technology, India (PDF/2015/000393). K.S.R. acknowledges N. G. Kantharia and Eric Greisen for valuable suggestions related to AIPS and M. S. Santhanam for valuable data analysis advice. P.S. acknowledges support from ISRO RESPOND program. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the staff of the Gauribidanur observatory for their help with the observations and maintenance of the antenna and receiver systems there. We thank the anonymous referee for an insightful report that has helped us improve the paper substantially.
Paper: 2016ApJ...832..203Z (acknowledgments)
H.J.Z. gratefully acknowledges the generous support of the Clay Postdoctoral Fellowship. M.J.G. and D.G.F. are supported by the Smithsonian Institution. We thank Scott Tremaine for carefully reading the manuscript and providing many useful comments. This work benefited from discussions with Ken Rines, Antonaldo Diaferio, Neta Bahcall, Mark Vogelsberger, and Paul Torrey. Masato Onodera kindly pointed out a mistake in Equation ( 5 ). This research has made use of NASA’s Astrophysics Data System Bibliographic Services. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.
Paper: 2016MNRAS.458L.104D (acknowledgments)
We thank the galform team for making the code publicly available. The work of ID and JS was supported by the ERC Project No. 267117 (DARK) hosted by Université Pierre et Marie Curie (UPMC) – Paris 6, PI J. Silk. JS acknowledges the support of the JHU by NSF grant OIA-1124403. The work of KAO was supported in part by DOE grant DE-SC0011842 at the University of Minnesota. This work has been carried out at the ILP LABEX (under reference ANR-10-LABX-63) supported by French state funds managed by the ANR within the Investissements d'Avenir programme under reference ANR-11-IDEX-0004-02.
Paper: 2018MNRAS.474..933R (acknowledgments)
Acknowledgements We thank Paul Benni and Tom Kaye for providing a few of the light curves and for helpful discussions. SR and BLG acknowledge partial support from National Aeronautics and Space Administration (NASA) Chandra grant GO7-18008X. AV was supported by the National Science Foundation (NSF) Graduate Research Fellowship, grant no. DGE 1144152, and also acknowledges partial support from NASA’s Transiting Exoplanet Survey Satellite (TESS) mission under a sub-award from the Massachusetts Institute of Technology to the Smithsonian Astrophysical Observatory, Sponsor Contract Number 5710003554. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute.
Paper: 2017MNRAS.468.1486D (acknowledgments)
Acknowledgments We thank C. Lang and D. Ludovici for sharing their reduced, high resolution VLA data covering the position of PSR J17462850, and G. Desvignes, R. Eatough, P. Esposito, D. Schnitzeler and A. Siemion for useful discussions. JD was supported by a Sofja Kovalevskaja Award from the Alexander von Humboldt Foundation of Germany. N. Degenaar acknowledges support via a Vidi grant from the Netherlands Organization for Scientific research (NWO) and a Marie Curie fellowship from the European Commission under contract no. FP-PEOPLE-2013-IEF-627148. J. Deneva was supported by the NASA Fermi program. MK and RK acknowledge the financial support by the European Research Council for the ERC Synergy Grant BlackHoleCam under contract no. 610058. The Parkes radio telescope is part of the Australia Telescope, which is funded by the Commonwealth Government for operation as a National Facility managed by CSIRO.
Paper: 2017ApJ...844..134L (fulltext)
(James et al. 2000 ). In this paper, we present the discovery of KELT J041621-620046, which is a bright ( J ∼ 10.2) 0.45 + 0.40 M eclipsing binary. This system is one of the brightest known detached M-M EB, with a very short orbital period of 1.11 days. With only about three dozen M-M EBs known, most with V > 14, KELT J041621-620046 provides the opportunity to test theoretical models for higher-mass M dwarfs. Section 2 presents the discovery photometry and the follow-up photometric and spectroscopic observations used. Section 3 presents the analysis and principal results of this study, including direct measurement of the two stars’ masses, radii, and other properties. In Section 4 , we briefly discuss the results in the context of the predictions of stellar models and of empirical relations for radius and temperature anomalies in LMSs. We summarize the results in Section 5 . 2. Observations 2.1. Kilodegree Extremely Little Telescope The Kilodegree Extremely Little Telescope (KELT) is an all-sky photometric survey designed to detect transiting planets around bright host stars (7 V 11). The survey uses two telescopes: the KELT-North in Soniata, AZ and the KELT-South at the South African Astronomical Observatory. Each telescope uses a 4096 × 4096 pixel Apogee CCD camera with a 42 mm aperture, producing a 26° × 26° field of view (Pepper et al. 2007 , 2012 ). See Kuhn et al. ( 2016 ) for a detailed description of the KELT-South data reduction pipeline. KELT J041621-620046 is located in KELT-South field 20, which is centered on J2000 α = 04 h 36 m 00 s δ = −53°00′00′′. KELT J041621-620046 itself is located at α = 04 h 16 m 21652 δ = −62°00′4644 J2000 and was observed by KELT-South 4182 times from UT 2010 February 28 until UT 2013 April 7. The discovery KELT light-curve is shown in Figure 1 . It is also known in various catalogs by the names 2MASS J04162165-6200463, UCAC4 140-003916, and WISE J041621.52-620047.1 (see Table 1 ). Figure 1. Top: the KELT-South light-curve of KELT J041621-620046 phase-folded to the discovery ephemeris ( T 0 = 2455255.950528 in JD TT , P = 1.1112884 days). The binned data are shown in red. Bottom: a zoom-in of the primary (left) and secondary (right) eclipses. The data used to create this figure are available . Table 1 Stellar Properties of KELT J041621-620046 Obtained from the Literature and from this Work Note. a See Zhou et al. ( 2015 ) for a description on how log( L H α / L bol ) was measured. 2.2. Photometric Follow-up To better measure the KELT J041621-620046 system, we obtained higher precision photometric follow-up of the primary and secondary eclipses from the KELT Follow-Up Network. All follow-up photometry except the Anglo-Australian Telescope (AAT) observations were reduced using the AstroImageJ 24 24 http://www.astro.louisville.edu/software/astroimagej (AIJ) package (Collins Kielkopf 2013 ; Collins et al. 2017 ) and the reported time stamps are BJD TDB . The AAT observations were reduced following the