adsabs/WIESP2022-NER huggingface dataset:
Paper: 2015ApJ...807..183L (acknowledgments)
The authors would like to thank Adam Burgasser, Brendan Bowler, Kelle Cruz, Mike Cushing, Michael Liu, and Emily Rice for useful discussions on benchmark systems, data treatment, and various data-model comparison approaches. The authors thank Richard Freedman and Roxana Lupu for providing gas opacities and Caroline Morley for radiative transfer code comparisons and helpful discussions. We thank Jacob Lustig-Yeager and Kyle Luther for rewriting portions of the code in python and C for significant speed improvements and also Dan Foreman-Mackey for making EMCEE available to the community. Finally, we thank the anonymous referee and statistics consultant for useful and insightful comments. J.T. acknowledges financial support from the Carnegie Origins Postdoctoral Fellowship Program. B.B. acknowledges financial support from the European Commission in the form of a Marie Curie International Outgoing Fellowship (PIOF-GA-2013-629435). J.F. acknowledges funding support from NSF award AST-1312545. M.M. acknowledges support from the NASA Astrophysics Theory and Planetary Atmospheres programs. Facility: Magellan:Clay
Paper: 2017MNRAS.468L..63B (acknowledgments)
Acknowledgments I thank Dustin Lang for providing the TGAS-matched APASS data, the 2016 NYC Gaia Sprint participants for stimulating discussions, and the anonymous referee for a helpful report. I also thank Maarten Breddels for finding and fixing a bug in Figs 2 and 3 . JB received support from the Natural Sciences and Engineering Research Council of Canada. JB also received partial support from an Alfred P. Sloan Fellowship and from the Simons Foundation. The MCMC analyses in this work were run using emcee (Foreman-Mackey etal. 2013 ). This project was developed in part at the 2016 NYC Gaia Sprint, hosted by the Center for Computational Astrophysics at the Simons Foundation in New York City. This work has made use of data from the European Space Agency (ESA) mission Gaia ( http://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research was made possible through the use of the APASS, funded by the Robert Martin Ayers Sciences Fund.
Paper: 2017A&A...602A..46J (acknowledgments)
The authors would like to thank their numerous colleagues for the many hours of fruitful discussions on the complex subject of interstellar dust. In particular we wish to thank Alain Abergel for a careful reading of the manuscript. This research was, in part, made possible through the financial support of the Agence National de la Recherche (ANR) through the programmes Cold Dust (ANR-07-BLAN-0364- 01) and CIMMES (ANR-11-BS56-0029) and, currently, through the EU FP7 funded project DustPedia (grant No. 606847).
Paper: 2017A&A...601A.129L (acknowledgments)
Work by J.D.L. and G.A.W. has been supported by the Natural Sciences and Engineering Research Council of Canada. O.K. acknowledges financial support from the Knut and Alice Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board. S.M. acknowledges funding by the European Research Council through ERC grant SPIRE 647383. S.M. thanks E. Bolmont for fruitful discussions on pseudo-synchronous states.
Paper: 2020MNRAS.492.2128P (acknowledgments)
ACKNOWLEDGEMENTS GAMA is a joint European–Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programs including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel -ATLAS, GMRT, and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/ . This work is based in part on observations made with the Galaxy Evolution Explorer (GALEX). GALEX is a NASA Small Explorer, whose mission was developed in cooperation with the Centre National d’Etudes Spatiales (CNES) of France and the Korean Ministry of Science and Technology. GALEX is operated for NASA by the California Institute of Technology, under NASA contract NAS5-98034. This work made extensive use of topcat (Taylor 2005 ) software packages, which are supported by an STFC grant to the University of Bristol.
Paper: 2015A&A...573A..38K (acknowledgments)
I thank all three anonymous referees, who reviewed this manuscript at different stages. I am also grateful to AA editor Malcolm Walmsley for his contribution in improving the presentation. This research has made use of NASA’s Astrophysics Data System.
Paper: 2019MNRAS.485..367K (acknowledgments)
ACKNOWLEDGEMENTS We thank the anonymous referee for a useful and supportive report. It is a pleasure to thank Mike Irwin for discussions on multiregression analysis. NK acknowledges the financial support from the Institute of Astronomy, Cambridge, the Nehru Trust for Cambridge University during the PhD, and the Schlumberger Foundation for the post-doctoral research. RM and MC acknowledge ERC Advanced Grant 695671 ‘QUENCH’ and support by the Science and Technology Facilities Council (STFC). This research has used the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; SAOImage DS9, developed by Smithsonian Astrophysical Observatory; Astropy, a community-developed core python package for Astronomy (Astropy Collaboration 2013 ). Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 095.B-0532(A), 096.B-0309(A), and 097.B-0165(A).
Paper: 2016MNRAS.463.2405A (acknowledgments)
We thank an anonymous referee for valuable comments that helped improve the paper. We thank Santiago García-Burillo for insightful discussions and Sebastian Hönig and Leonard Burtscher for making their fully reduced spectra available to us. We acknowledge financial support from the Spanish Ministry of Economy and Competitiveness through the Plan Nacional de Astronomía y Astrofísica grants AYA2012-31447 (AA-H and AH-C), and AYA2015-64346-C2-1-P (AA-H), which were partly funded by the FEDER programme, and AYA2015-70815-ERC and AYA2012-31277 (AH-C) and AYA2012-32295 (MP-S and LC). AA-H is also partly funded by CSIC/PIE grant 201650E036. RP acknowledges the Oxford University Summer Research Programme. IA and MM-P are partly supported by Mexican CONACyT through research grant CB-2011-01-167291. MM-P acknowledges support by the CONACyT PhD fellowship programme. CRA acknowledges the Ramón y Cajal Programme of the Spanish Ministry of Economy and Competitiveness. NAL is supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Brazil, Canada, Chile, and the United States of America. TD-S acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT 1151239. Based on observations made with the GTC, installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. This research has made use of the NED which is operated by JPL, Caltech, under contract with the National Aeronautics and Space Administration. This work is based in part on observations made with the Spitzer Space Telescope , which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.
Paper: 2016ApJ...823...14T (acknowledgments)
K.O.T., M.R.M., and S.P.Q. gratefully acknowledge the support of the Swiss National Centers of Competence in Research (NCCR) PlanetS initiative, funded by the Swiss National Science Foundation. This research made use of NASA's Astrophysics Data System. This research made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org . This research benefitted from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://pono.ucsd.edu/adam/browndwarfs/spexprism .
Paper: 2017ApJ...835..267H (acknowledgments)
This research was partially supported by the National Science Foundation under AST-1109288. G.G.K. acknowledges the support of the Australian Research Council through the award of a Future Fellowship (FT140100933). We thank the referee for useful suggestions. We thank Mark Seibert for the discussion on GALEX photometry. We gratefully acknowledge conversations with Peng Oh and Andrey Kravtsov, which contributed to shaping our interpretation of these data. Most of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some presented data are based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. Facilities: Keck:I (LRIS) , Keck:II (NIRC2) , Gemini:Gillett (GMOS) , GALEX , ARC.
Paper: 2015ApJ...801....3M (acknowledgments)
We are indebted to the referee for very thoughtful advice that substantially improved the previous version of the paper. We wish to deeply thank Tomer Holczer for his tests to identify EB contamination, Gil Nachmani, Suzanne Aigrain and Simchon Faigler for illuminating and helpful discussions, and Eric Agol for useful comments. The research leading to these results has received funding to T.M. from the European Research Council under the EU's Seventh Framework Programme (FP7/(2007-2013)/ERC grant agreement No. 291352). T.M. also acknowledges support from the Israel Science Foundation (grant No. 1423/11). T.M. and H.B.P. acknowledge support from the Israeli Centers of Research Excellence (I-CORE, grant No. 1829/12). H.B.P. acknowledges support from the European Union's—Seventh Framework Programme (FP7/2007-2013]) under grant agreement No. 333644–MC–GRAND, as well as the “Minerva center for life under extreme planetary conditions.” T.M. is grateful to the Jesus Serra Foundation that enabled an extended visit to the Instituto de Astrofísica de Canarias, and to his hosts, Hans Deeg and Rafael Rebolo in particular. The last phase of this work has been completed during this visit. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. All 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: 2015MNRAS.454L..21C (acknowledgments)
We used data from the DASCH project, which is supported by the NSF grant AST-1313370. The analysis was performed using the HPC Cluster Yeti at Columbia University.
Paper: 2017ApJ...847...44Q (acknowledgments)
We acknowledge the anonymous referee for suggestions regarding the phase-connection analysis and the position accuracy. We thank Peng Wei and Eugene Magnier for helpful discussion about the search of the optical/IR counterpart. This work was supported by NSFC grants 11503008 and J1210039, and Top-notch Academic Programs Project of Jiangsu Higher Education Institutions. P.Z. acknowledges the support from the NWO Veni Fellowship, grant No. 639.041.647, and NSFC grant 11233001. W.Y. was supported in part by NSFC grant No. 11333005 and by the National Program on Key Research and Development Project (grant No. 2016YFA0400804). X.L. was supported by the National Program on Key Research and Development Project (grant No. 2016YFA0400803), and NSFC grants 11133001 and 11333004. X.X. is grateful for the support of NSFC grant 11303015.
Paper: 2016A&A...587A.154S (acknowledgments)
Rosetta is a European Space Agency (ESA) mission with contributions from its member states and the National Aeronautics and Space Administration (NASA). This study was supported by the Academy of Finland and, in part, by the Research Council of Norway grant No. 240000. The work on RPC-ICA was funded by the Swedish National Space Board under contracts 108/12 and 112/13. Work at the Belgian Institute for Space Aeronomy was supported by the Belgian Science Policy Office through the Solar-Terrestrial Centre of Excellence and by PRODEX/ROSETTA/ROSINA PEA 4000107705. First selection of events in this study was performed with the AMDA science analysis system provided by the Centre de Données de la Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and Université Paul Sabatier, Toulouse. G.G. is supported by the NASA Astrobiology Institute Grant NNX15AE05G and by the NASA HIDEE program Grant NNH15CO73C. C.S.W. thanks T.E. Cravens (University of Kansas, USA), W.J. Miloch (University of Oslo, Norway) and, last but not least, M. Simon Wedlund for useful discussions.
Paper: 2016ApJ...818..172G (acknowledgments)
This research was supported under the Australian Research Councils funding scheme (FT110100263). This research has made use of the NASA/IPAC Extragalactic Database (NED). 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.
Paper: 2017MNRAS.466.1669Y (acknowledgments)
We would are deeply grateful to our colleagues who have provided us with valuable guidance. Special thanks to Professor Cui X. Q. (NIAOT) and Professor Granham J. Murray (Durham University) for productive discussions. Without their enlightening instruction, impressive kindness and patience, this paper could not have been completed. The Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope, LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences.
Paper: 2019A&A...629A..74G (acknowledgments)
We wish to commemorate our colleague and friend Gregory Ruchti (1980–2019) who originally branched off this pipeline from the LUMBA-internal GIRAFFE pipeline. We thank the GES team for the work behind the M 67 spectra and for making them available to us. We thank Caroline Soubiran, Paula Jofré, and Maria Bergemann for contributions to the work behind the pipeline. AG, UH, and AJK acknowledge support from the Swedish National Space Agency and the Knut and Alice Wallenberg Foundation. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. PG thanks the European Science Foundation (ESF) for support in the framework of EuroGENESIS. KL acknowledges funds from the Alexander von Humboldt Foundation in the framework of the Sofja Kovalevskaja Award endowed by the Federal Ministry of Education and Research and funds from the Swedish Research Council (Grant no. 2015-00415_3 ) and Marie Skłodowska Curie Actions (Cofund Project INCA 600398). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
Paper: 2018A&A...618A...3R (acknowledgments)
The authors would like to thank the anonymous referee for helping to improve the quality of this paper. SK, PMW, and CS received funding through BMBF Verbundforschung (grants 05A14BAC, 05A14MGA, ERASMUS-F, grant 05A08BA1, and ELT-MOS, grant 05A15BA1). SD acknowledges BMBF support through grant 05A14MGA, and from DFG through DR281/35-1. AMI acknowledges support from the Spanish MINECO through project AYA2015-68217-P. MMR acknowledges fruitful discussions with PER and TJR. The authors are thankful to A. Vazdekis for providing the (unpublished) MIUSCAT library. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space TelescopevScience Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This research has made use of the Spanish Virtual Observatory ( http://svo.cab.inta-csic.es ) supported from the Spanish MINECO/FEDER through grant AyA2014-55216.
Paper: 2017ApJ...839..116A (acknowledgments)
The research leading to the presented results has received funding from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no 338251 (StellarAges). E.B. undertook this research in the context of the International Max Planck Research School for Solar System Research. S.B. acknowledges partial support from NSF grant AST-1514676 and NASA grant NNX13AE70G. We thank Alexy Mints and the anonymous referee for their useful comments and discussions, which helped improve this manuscript. Software: Stellar models were calculated with Modules for Experiments in Stellar Astrophysics r8118 (MESA, Paxton et al. 2011 ) and stellar oscillations with the ADIPLS pulsation package 0.2 (Christensen-Dalsgaard 2008 ). Analysis in this manuscript was performed with python 3.5.1 libraries scikit-learn 0.17.1 (Pedregosa et al. 2011 ), NumPy 1.11.0 (Van Der Walt et al. 2011 ), matplotlib 1.5.1 (Hunter 2007 ), biokit 0.3.2 16 16 T. Cokelaer et al. 2016, (Version 0.3.2), https://github.com/biokit/biokit , and pandas 0.19.0 (McKinney 2010 ) as well as R 3.3.2 (R Core Team 2014 ) and the R libraries magicaxis 2.0.0 (Robotham 2015 ), RColorBrewer 1.1-2 (Neuwirth 2014 ), parallelMap 1.3 (Bischl Lang 2015 ), data.table 1.9.6 (Dowle et al. 2015 ), ggplot2 2.1.0 (Wickham 2009 ), GGally 1.2.0 (Schloerke et al. 2014 ), scales 0.4.0 (Wickham 2015 ) and Corrplot 0.77.
Paper: 2019ApJ...875...39B (acknowledgments)
We thank the anonymous referee for comments that significantly improved the manuscript. We additionally thank X. Bai, R. Fu, and J. Bryson for useful discussions. We gratefully acknowledge support from the NASA Emerging Worlds program (grant No. NNX15AH72G) , the U.S. Rosetta program (CREI 1576768), and Thomas F. Peterson Jr. Software: Astropy (Astropy Collaboration et al. 2013 ), matplotlib (Hunter 2007 ), NumPy (Van Der Walt et al. 2011 ), SciPy (Jones et al. 2001 ).
Paper: 2017A&A...601A.122D (acknowledgments)
This work has benefited from the discussions at the meeting “Solar UV bursts – a new insight to magnetic reconnection” at the International Space Science Institute (ISSI) in Bern. NASA’s Astrophysics Data System (ADS) and the 3D visualization tool Vapor were extensively used in this study.
Paper: 2017ApJ...851....3V (acknowledgments)
SDO is a mission of NASA’s Living With a Star Program. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. I thank the referee for specific comments and suggestions that improved the scientific presentation of the content. P.V. is supported by an INSPIRE grant of AORC scheme under the Department of Science and Technology. I am thankful to Prof. P. Venkatakrishnan for introducing me to this problem of net current neutralization.
Paper: 2015MNRAS.446.2952C (acknowledgments)
We appreciate Professor L. Perivolaropoulos for useful discussions. We are grateful to M.-H. Li, X. Li and S. Wang for meaningful suggestions. This work has been funded by the National Natural Science Fund of China under Grant no. 11375203.
Paper: 2019MNRAS.482.1143H (acknowledgments)
ACKNOWLEDGEMENTS The authors would like to thank both Andrew Gilbert and the anonymous referee for their comments that greatly improved the content of the manuscript. AH is supported by his STFC Ernest Rutherford Fellowship grant number ST/L00397X/2 and by STFC grant ST/R000891/1. AB was supported by the Leverhulme Trust through the award of an Early Career Fellowship and by STFC Grant ST/R00059X/1. IA acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) through projects AYA2014-55456-P (Bayesian Analysis of the Solar Corona), AYA2014-60476-P (Solar Magnetometry in the Era of Large Telescopes), from FEDER funds, and through a Ramon y Cajal fellowship.
Paper: 2018ApJ...853...80A (acknowledgments)
Support from the Junta de Extremadura (Research Group Grant GR15137) and from the Ministerio de Economía y Competitividad of the Spanish Government (AYA2014-57556-P) is gratefully acknowledged. I.U. acknowledges support by the Center of Excellence ReSoLVE (Academy of Finland Project No. 272157).
Paper: 2018MNRAS.477..153A (acknowledgments)
ACKNOWLEDGEMENTS C.A. would like to acknowledge support by the NSF research grant AST-1613472. M.D.S. acknowledges support by a research grant (13261) from VILLUM FONDEN. The work presented in this paper has been supported in part by NSF awards AST-1613472 (PI: E. Y. Hsiao), P. Hoeflich AST-1715133 (PI: P. Hoeflich), and AST-1613426 (PI: M. M. Phillips). We also acknowledge the Florida Space Grant Consortium. C.G. acknowledges support by the Carlsberg Foundation. The UCSC team is supported by NSF grant AST-1518052, the Gordon Betty Moore Foundation, and from fellowships from the Alfred P. Sloan Foundation and the David and Lucile Packard Foundation to R.J.F. Support for programme #GO–12592 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555.
Paper: 2017ApJ...849..156C (acknowledgments)
E.C. acknowledges financial support from the Chinese Academy of Sciences Presidents’ International Fellowship Initiative, Grant No. 2015PM054. E.C., X.K., and A.R. acknowledge financial support by the 973 program (No. 2015CB857003, 2013CB834900), NSF of Jiangsu Province (No. BK20140050), and the NSFC (No. 11333008, 11550110182, 11550110183). E.C. and S.K.Y. acknowledge support from the Korean National Research Foundation (NRF-2017R1A2A1A05001116) and from the Brain Korea 21 Plus Program (21A20131500002). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute.