adsabs/WIESP2022-NER huggingface dataset:
Paper: 2015A&A...575A.112D (acknowledgments)
We want to thank the referee for his/her useful and constructive comments. This work is supported by ANPCyT (PICT 2012-00878). V.B-R. acknowledges financial support from MICINN and European Social Funds through a Ramón y Cajal fellowship. This research has been supported by the Marie Curie Career Integration Grant 321520. V.B-R. and G.E.R. acknowledge support by the Spanish Ministerio de Economía y Competitividad (MINECO) under grant AYA2013-47447-C3-1-P.
Paper: 2015ApJ...807...45D (acknowledgments)
C.D. is supported by a National Science Foundation Graduate Research Fellowship. Support for this work was provided through the NASA Kepler Mission Participating Scientist Program grants NNX09AB53G and NNX12AC77G, which were awarded to D.C. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. We thank the anonymous referee for providing feedback that improved the quality of this paper and the Kepler team for providing the community with a fantastic collection of data. We are grateful to Jonathan Irwin for sharing a fast implementation of the transit model (Mandel Agol 2002 ) and for providing valuable advice. We thank Jessie Christiansen for answering questions about the Kepler pipeline completeness and providing helpful suggestions. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This publication made use of the Kepler Community Follow-Up Observing Program website ( https://cfop.ipac.caltech.edu ), the NASA Exoplanet Archive, and the Mikulski Archive for Space Telescopes (MAST). The NASA Exoplanet Archive is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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: 2017MNRAS.467.3454B (acknowledgments)
Acknowledgments We thank Christoph Behrens for providing the MDPL2 merger trees in the galacticus merger tree file format, and Shaun Cole and Yu Lu for helpful discussions. The author gratefully acknowledges the Gauss Centre for Supercomputing e.V. ( www.gauss-centre.eu ) and the Partnership for Advanced Supercomputing in Europe (PRACE, http://www.prace-ri.eu ) for funding the MultiDark simulation project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (LRZ, http://www.lrz.de ). The CosmoSim data base used in this paper is a service by the Leibniz Institute for Astrophysics Potsdam (AIP). The MultiDark data base was developed in cooperation with the Spanish MultiDark Consolider Project CSD2009-00064.
Paper: 2019A&A...622A.165D (acknowledgments)
LD and JS acknowledge support from the ESA PRODEX Programme “ Gaia -DPAC QSOs” and from the Belgian Federal Science Policy Office. AKM acknowledges the support from the Portuguese Fundação para a Ciência e a Tecnologia (FCT) through grants SFRH/BPD/74697/2010 and PTDC/FIS-AST/31546/2017, from the Portuguese Strategic Programme UID/FIS/00099/2013 for CENTRA, from the ESA contract AO/1-7836/14/NL/HB, and from the Caltech Division of Physics, Mathematics and Astronomy for hosting a research leave during 2017–2018, when this paper was prepared. OW is supported by the Humboldt Research Fellowship for Postdoctoral Researchers. SGD and MJG acknowledge partial support from the NSF grants AST-1413600 and AST-1518308, and the NASA grant 16-ADAP16-0232. The work of DS was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We acknowledge partial support from “Actions sur projet INSU-PNGRAM”, and from the Brazil-France exchange programmes Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) and Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) – Comité Français d’Évaluation de la Coopération Universitaire et Scientifique avec le Brésil (COFECUB). This work has made use of the computing facilities of the Laboratory of Astroinformatics (IAG/USP, NAT/Unicsul), whose purchase was made possible by the Brazilian agency FAPESP (grant 2009/54006-4) and the INCT-A, and we thank the entire LAi team, especially Carlos Paladini, Ulisses Manzo Castello, Luis Ricardo Manrique, and Alex Carciofi for their support. This work has made use of results from the ESA space mission Gaia , the data from which were processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Gaia mission website is http://www.cosmos.esa.int/gaia . Some of the authors are members of the Gaia Data Processing and Analysis Consortium (DPAC).
Paper: 2017ApJ...838..130S (acknowledgments)
We thank A. Rubin, B. Katz, E. Ofek, and A. Gal-Yam for useful discussions and constructive comments. This research was partially supported by an ISF I-Core, an IMOS grant, and a Minerva grant.
Paper: 2017MNRAS.470.2351W (acknowledgments)
Acknowledgments WW is grateful for useful discussions of merger trees with John Helly and Yan Qu. WW also thank Azadeh Fattahi and Shi Shao about the useful information of apostle . This work was supported by the European Research Council [GA 267291] COSMIWAY and Science and Technology Facilities Council Durham Consolidated Grant [ST/F001166/1,ST/L00075X/1]. WW acknowledges a Durham Junior Research Fellowship (RF040353). The simulations for the Aquarius project were carried out at the Leibniz Computing Centre, Garching, Germany, at the Computing Centre of the Max-Planck-Society in Garching, at the Institute for Computational Cosmology in Durham and on the STELLA supercomputer of the LOFAR experiment at the University of Groningen. apostle project used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility ( www.dirac.ac.uk ), and also resources provided by WestGrid ( www.westgrid.ca ) and Compute Canada ( www.computecanada.ca ). The DiRAC system was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grants ST/H008519/1 and ST/K00087X/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. Kavli IPMU was established by World Premier International Research Center Initiative (WPI), MEXT, Japan. This work was supported by JSPS KAKENHI Grant Number JP17K14271.
Paper: 2016ApJ...823...96R (acknowledgments)
A.R.L. is grateful for partial support from DIULS Regular project PR15143. G.A.P.F. is partially supported by CNPq and FAPEMIG. We thanks the SOAR staff for the efficient support provided during the OSIRIS and Goodman observing runs. A.R.L. thanks Dr. Nolan Walborn for stimulating discussions about the optical spectra of O2 v stars. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. 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. This research has made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in AAS 143, 23 Facility : OSIRIS.
Paper: 2017A&A...602A...3D (acknowledgments)
The authors are grateful to the anonymous referee for his/her careful reading and useful comments, which improved the content of this manuscript. I.D., V.S., J.D., M.N., and O.M. acknowledge the European Union’s Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, “CoSMass”). N.B. acknowledges the European Union’s Seventh Framework programme under grant agreement 333654 (CIG, “AGN feedback”). C.L. is funded by a Discovery Early Career Researcher Award (DE150100618). Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. M.B. and P.C. acknowledge supports from the PRIN-INAF 2014. M.A. acknowledges partial support from FONDECYT through grant 1140099. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). This work was partially supported by NASA Chandra grant number GO3-14150C and GO3-14150B (FC, S.M.). I.D. is grateful to B. Magnelli for useful suggestions and to Takamitsu Miyaji for his help with CSTACK.
Paper: 2017MNRAS.467..226G (acknowledgments)
Acknowledgments I am most grateful to Ski Antonucci and Bill Mathews for numerous comments and discussions. I have also benefitted considerably from discussions of hydrogen-line ratios with Gary Ferland, and discussions of AGN reddening and dust issues with Victor Oknyansky, Clio Heard and Jonathan Stern.
Paper: 2017MNRAS.467...50N (acknowledgments)
Acknowledgments The authors thank Thomas Bisbas, Tanio Diaz-Santos, Duncan Farrah, Munan Gong, Javier Gracia-Carpio and Eve Ostriker for providing both simulation and observational data that aided us when developing these models. DN thanks Aaron Evans, Thomas Greve, Rob Kennicutt, Dominik Riechers, J. D. Smith, Gordon Stacey, Dan Stark, Karen Olsen and Mark Wolfire for helpful conversations. Partial support for DN was provided by NSF AST-1009452, AST-1445357, NASA HST AR-13906.001 from the Space Telescope Science Institute, which is operated by the Association of University for Research in Astronomy, Incorporated, under NASA Contract NAS5-26555, and a Cottrell College Science Award, awarded by the Research Corporation for Science Advancement. MRK acknowledges support from US NSF grant AST-1405962 and Australian Research Council grant DP160100695.
Paper: 2015A&A...584A..47R (acknowledgments)
We thank the anonymous referee for constructive comments that helped us to improved the manuscript. This work was funded with grants from Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina and the Universidad Nacional de La Plata (Argentina).
Paper: 2020ApJ...888...86Z (acknowledgments)
We thank Feng Yuan for his thoughtful and constructive comments. Amin Mosallanezhad is supported by the Chinese Academy of Sciences President’s International Fellowship Initiative (PIFI), grant No. 2018PM0046. This work is supported by the National Natural Science Foundation of China (grant No. 11725312, 11421303), the Science Challenge Project of China (grant No. TZ2016002), and the China Postdoctoral Science Foundation (grant No. 2019M663665).
Paper: 2017ApJ...845..146H (acknowledgments)
We thank Peter Stetson for a copy of DAOPHOT as well as his helpful engagement on its usage. We also thank C. Gallart and M. Monelli of the LCID team for a copy of their IC 1613 photometric catalog for comparison to our own. We also thank Richard Kron for helpful comments in this research and preparation of this manuscript, Julia Kollmeier for helpful conversations, and Laura Sturch for the preparation of IMACS imaging. In addition, we thank the anonymous referee for numerous constructive suggestions. Authors M.G.L. and I.S.J. were supported by the National Research Foundation of Korea (NRF) grant funded by the Korea Government (MSIP) No. 2012R1A4A1028713. Support for program #13691 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. This research has made use of 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. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. We thank the Carnegie Institution for its continued support of this program over the past 30 years. Facilities: HST (ACS/WFC , WFC3-IR) , Magellan-Baade (IMACS) . Software: DAOPHOT (Stetson 1987 ), ALLFRAME (Stetson 1994 ), Tiny Tim (Krist et al. 2011 ).
Paper: 2018MNRAS.475.3273P (acknowledgments)
ACKNOWLEDGEMENTS I am grateful to the anonymous reviewer for justified, helpful, and clearly rationalized remarks that helped improve this paper.
Paper: 2015ApJ...806..257M (acknowledgments)
C.-J.M. acknowledges support from ERC Advanced Investigator programme DUSTYGAL 321334. I.R.S. acknowledges support from STFC (ST/L00075X/1), the DUSTYGAL ERC programme, and a Royal Society/Wolfson Merit Award. A.M.S. acknowledges an STFC Advanced Fellowship through grant number ST/H005234/1 and the Leverhume Trust. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and (until 2013 March 31) the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of NASA’s Astrophysics Data System.
Paper: 2015ApJ...804....4K (acknowledgments)
We would like to thank the referee for constructive and valuable comments that improved the manuscript considerably. SDO is a mission for NASA’s Living With a Star (LWS) program. P. K. thanks Prof. Davina Innes for several fruitful discussions. We acknowledge the use of the Fermi Solar Flare Observations facility funded by the Fermi GI 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. It is operated by these agencies in cooperation with the ESA and the NSC (Norway). This work was supported by the “Development of Korea Space Weather Center” of KASI and the KASI basic research funds. V. M. N. acknowledges support from the European Research Council under the SeismoSun Research Project No. 321141, STFC consolidated grant ST/L000733/1, and the BK21 Plus Program through the National Research Foundation funded by the Ministry of Education of Korea.
Paper: 2016MNRAS.456.2425V (acknowledgments)
We thank the anonymous referee for a critical reading of the manuscript and highly appreciate the comments and suggestions, which significantly contributed to improving quality of the paper. We also thank the staff of GMRT, who made the radio observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. We thank UKIRT staff for their assistance in observations. The UKIRT is supported by NASA and operated under an agreement among the University of Hawaii, the University of Arizona and Lockheed Martin Advanced Technology Center; operations are enabled through the cooperation of the Joint Astronomy Centre of the Science and Technology Facilities Council of the UK. When the data reported here were acquired, UKIRT was operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. We thank the Mt. Abu Infrared Observatory staff for assistance in the observations. We also thank M. T. Beltran for providing the 1.2 mm map of this region. We thank A. Sanchez-Monge for providing the ATCA maps. We also thank Varsha Ramachandran and Govind Nandakumar for their help in python programming. This research made use of NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, Caltech under contract with NASA. This publication also made use of data products from Herschel (ESA space observatory). We use ATLASGAL [collaboration between the Max-Planck-Gesellschaft, the European Southern Observatory (ESO) and the Universidad de Chile] data products for our research.
Paper: 2019ApJ...871....8L (acknowledgments)
The research was supported by NSFC under grant 41774179 and the Specialized Research Fund for State Key Laboratories of China. We acknowledge the use of data from SOHO , STEREO , SDO , GOES , Wind , and MAVEN , we thank M. Leila Mays, Christina O. Lee and Janet G. Luhmann for their help and discussions on the work, and we are grateful to R.-Y. Kwon for providing his ellipsoidal shock model. The ENLIL simulations were provided by CCMC through their public Runs on Request system ( http://ccmc.gsfc.nasa.gov ).
Paper: 2017ApJ...834..181O (acknowledgments)
Thanks are due to R. Amorín, Y. Ascasibar, A. B. Morales-Luis, P. Papaderos, and J. Vílchez, who participated in the target selection and in some of the observing time proposals that produced the spectra analyzed in the paper. We also thank an anonymous referee whose comments helped to improve the readability of the paper. This article is based on observations made with the WHT operated by the ING in the Observatorio del Roque de los Muchachos, La Palma, Spain. This work has been partly funded by the Spanish Ministry of Economy and Competitiveness, projects Estallidos AYA2013–47742–C04–02–P and AYA2013–47742–C04–01–P. A.O.-G. thanks Fundación La Caixa for financial support in the form of a PhD contract. M.E.F. is partly funded by the Estallidos project, as well as by the Fundao para a Cincia e Tecnologia (FCTPortugal), through the research grant SFRH/BPD/107801/2015. J.M.-A. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild).
Paper: 2016MNRAS.458.1939B (acknowledgments)
The simulations have been carried out either on a work station with multicore processors or/and on the CFCA cluster (XC30) of National Astronomical Observatory of Japan. We make 2D visualization and analysis using package visit (Childs et al. 2012 ) and octave . SSK acknowledges support by STFC under the standard grant EP/N023986/1. BMV acknowledge partial support by JSPS (Japan Society for the Promotion of Science): No.2503786, 25610056, 26287056, 26800159. BMV also MEXT (Ministry of Education, Culture, Sports, Science and Technology): No.26105521 and RFBR grant 12-02-01336-a.
Paper: 2017MNRAS.468.3737K (acknowledgments)
Acknowledgments We thank Simon White and Philipp Busch for helpful input to the analysis.
Paper: 2015ApJ...814...11T (acknowledgments)
The authors thank an anonymous referee for constructive comments that improved the clarity of the paper. This research is based on observations obtained with XMM-Newton , an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and AKARI , a JAXA project with the participation of ESA. This research made use of 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, and the HyperLeda database ( http://leda.univ-lyon1.fr ). Facilities: XMM-Newton , AKARI
Paper: 2017A&A...604A.135D (acknowledgments)
We wish to thank an anonymous referee for his/her many interesting comments and suggestions. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES-UVES reduction team at INAF-Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia -ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 program through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell’ Istruzione, dell’ Università’ e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012”. T.Z. acknowledges support from the Slovenian Research Agency (research core funding No. P1-0188). F.J.-E. acknowledges financial support from the Spacetec-CM project (S2013/ICE-2822). M.T.C. acknowledges the financial support from the Spanish Ministerio de Economía y Competitividad, through grant AYA2016-75931-C2-1-P. The results presented here benefit from discussions held during the Gaia -ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. This work is also based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 177.D-3023, as part of the VST Photometric H Survey of the Southern Galactic Plane and Bulge (VPHAS, www.vphas.eu ). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
Paper: 2019MNRAS.485.3794D (acknowledgments)
ACKNOWLEDGEMENTS This study uses data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey ( http://califa.caha.es/ ). Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). IMC acknowledges the support of the Instituto de Astrofísica de Canarias via an Astrophysicist Resident fellowship. BGL acknowledges support from the Spanish Ministerio de Economia y Competitividad (MINECO) by the grant AYA2015-68217-P. CRA acknowledges the Ramón y Cajal Program of the Spanish Ministry of Economy and Competitiveness through project RYC-2014-15779 and the Spanish Plan Nacional de Astronomía y Astrofisíca under grant AYA2016-76682-C3-2-P. TRL acknowledges support via grants AYA2014-56795-P and AYA2016-77237-C3-1-P from the Spanish Government. JFB acknowledges support from the Spanish Ministerio de Economia y Competitividad (MINECO) by the grant AYA2013-48226-C3-1P. SFS thanks the CONACyT programs CB-285080 and DGAPA IA101217 grants for their support. IMP and JM acknowledges support from the Spanish Ministerio de Economia y Competitividad(MINECO) by the grant AYA2016-76682-C3-1-P. This paper makes use of python ( http://www.python.org ); Matplotlib (Hunter 2007 ), a suite of open-source python modules that provide a framework for creating scientific plots; and Astropy, 6 a community-developed core python package for Astronomy (Astropy Collaboration et al. 2013 , 2018 ). Finally, we thank the anonymous referee for useful suggestions and comments that have improved this paper.