adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017ApJ...843..125J (acknowledgments)
We thank our collaborators as well as the anonymous referee for constructive comments that improved the paper. This work was supported in part by the National Aeronautics and Space Administration under grant number NNX15AU32H issued through the NASA Education Minority University Research Education Project (MUREP) through the NASA Harriett G. Jenkins Graduate Fellowship activity. R.C.H. acknowledges support from the National Science Foundation through CAREER grant number 1554584. This research has made use of NASA’s Astrophysics Data System.
Paper: 2015A&A...577A..77S (acknowledgments)
We wish to thank the anonymous referee for the extremely useful comments. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. This work was partly supported by the European Union FP7 programme 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”. 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. We wish to thank C. Bailer-Jones and C. Babusiaux for extremely useful comments. M. Schultheis, A. Recio-Blanco, P. de Laverny, and V. Hill acknowledge the support of the “Programme National de Cosmologie et Galaxies” (PNCG) of CNRS/INSU, France. T.B. is funded by grant No. 621-2009- 3911 from the Swedish Research Council.
Paper: 2017MNRAS.464.2174B (acknowledgments)
We thank Karl Gebhardt, Georges Meylan, Ben MacLean and Sandro Villanova for sharing unpublished radial velocity data with us. We are also grateful to Long Wang for sending us data from his simulations. We finally thank Pouria Khalaj and two anonymous referees for comments that helped improve the presentation of the paper. This work has made use of BaSTI web tools.
Paper: 2017MNRAS.466.1757K (acknowledgments)
We thank Dmitrii Barsukov, Serge Balashev and Aida Kirichenko for discussions. The work was supported by the Russian Science Foundation, grant 14-12-00316. For Fig. 6 we used the data from the VGPS survey conducted by the National Radio Astronomy Observatory (NRAO) instruments. NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.
Paper: 2017A&A...597A...4S (acknowledgments)
This research was funded by the European Union’s Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, “CoSMass”). A.F. wishes to acknowledge Finnish Academy award, decision 266918. This work was supported in part by the National Science Foundation under Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. This work is partly based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and and 185.A-0791 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This research has made use of NASA’s Astrophysics Data System, and the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the NASA. We greatfully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos . We thank the VUDS team for making the data in the COSMOS field available prior to public release.
Paper: 2015ApJ...798...11P (acknowledgments)
We would like to acknowledge the continual assistance with the Hyperion code from Dr. Thomas Robitaille and the useful discussions with Brian Kloppenborg and Kathy Geise. We thank the referee for useful comments and suggestions. This work was supported in part by the bequest of William Herschel Womble in support of astronomy at the University of Denver, as well as a Grant-In-Aid of Research from the National Academy of Sciences, administered by Sigma Xi, The Scientific Research Society, for which we are grateful.
Paper: 2016A&A...590A..64S (acknowledgments)
We thank the referee for comments that pushed us to improve the analysis of Sect. 3.3. S.C. warmly thanks the financial support by PRIN-INAF2014 (PI: S. Cassisi) and the Economy and Competitiveness Ministry of the Kingdom of Spain (grant AYA2013-42781-P). A.P. acknowledges financial support by PRIN-INAF 2012 The M4 Core Project with Hubble Space Telescope (P.I.: L. Bedin).
Paper: 2020MNRAS.492.4945B (acknowledgments)
ACKNOWLEDGEMENTS We are grateful to Ling Sun, Joe Romano, David Keitel, and Paul Schale for useful discussion and comments. We also thank Tyson Littenberg for insightful comments and suggestions that improved the paper. SB acknowledges support by the Hoff Lu Fellowship at the University of Minnesota, and by NSF grant PHY-1806630. MWC is supported by the David and Ellen Lee Postdoctoral Fellowship at the California Institute of Technology. PDL is supported by ARC Future Fellowship FT160100112 and ARC Discovery Project DP180103155. ET and CT are supported by CE170100004. ET is supported by FT150100281. The authors are thankful for the computing resources provided by LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058. All posterior corner plots were made with ChainConsumer (Hinton 2016 ). The code for the analysis in this paper is available upon request. A public release is being planned for the near future. This paper has been assigned document number LIGO-P1900107.
Paper: 2018ApJ...863..199G (acknowledgments)
We greatly appreciate the lengthy conversations with Cole Miller regarding the development of the MCMC code. We thank the referee for carefully reading the manuscript and providing many helpful comments that led to its improvement. This research was supported in part by the Howard Hughes Medical Institute through the Undergraduate Science Education Program. We also are grateful for the generous support of the Michigan Space Grant Consortium, the National Science Foundation under Grant Nos. REU: PHY/DMR-1004811 and RUI: AST-1009731, the Fermi Guest Investigator Program Cycle 3 under Grant No. NNH09ZDA001N-FERMI3, and the NASA Astrophysics Theory and Fundamental Physics Program under Grant No. NNX13AO12G.
Paper: 2016A&A...588A.149K (acknowledgments)
S.K. and P.M.W. received funding through BMBF Verbundforschung (project MUSE-AO, grant 05A14BAC and 05A14MGA). S.K. further acknowledges support from DFG via SFB 963/1 “Astrophysical flow instabilities and turbulence” (project A12).
Paper: 2019MNRAS.486.2063H (acknowledgments)
ACKNOWLEDGEMENTS We would like to thank the referee for providing a clear, constructive, and concise report that greatly improved the interpretations presented here. We would also like to thank Karl Gordon for an enlightening discussion in the early stages of this work. KEH and PJ acknowledge support by a Project Grant (162948-051) from The Icelandic Research Fund. The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF).
Paper: 2015MNRAS.447.2181I (acknowledgments)
It is a pleasure to thank the anonymous referee for their positive and helpful suggestions. NI thanks NSERC Discovery and Canada Research Chairs Program. SJ thanks the Chinese Academy of Sciences and National Science Foundation of China, project numbers 11250110055 and 11350110324. PhP thanks the Umezawa Fund for hospitality. This work was supported in part by the National Science Foundation under Grant no. NSF PHY11-25915, Grant no. PHYS-1066293 and the hospitality of the Aspen Center for Physics.
Paper: 2017ApJ...851..129N (acknowledgments)
This research was supported by the Russian Foundation for Basic Research (grant No. 15-02-06079), by the Grants Council under the President of the Russian Federation (grant No. MK-2218.2017.2), and by the “Basis” Foundation (grant No. 17-11-101). We thank Vl. V. Kocharovsky for inspiring conversations and I. I. Artemenko for a discussion on the effect of collisions. Software: quill (Nerush Kostyukov 2010 ; Serebryakov et al. 2015 ; http://iapras.ru/english/structure/dep_330/quill.html ), ggplot2 (Wickham 2016 ; http://ggplot2.org/ ).
Paper: 2015ApJ...808...63H (acknowledgments)
The authors wish to thank Dr. Kevin Walsh and Dr. Dan Durda at SwRI Boulder, Dr. Dave Jewitt at UCLA, and Dr. Tony Dobrovolskis at SETI Institute for useful comments on the present work.
Paper: 2017MNRAS.464.4823B (acknowledgments)
This research is part of the project GLENCO, funded under the European Seventh Framework Programme, Ideas, Grant Agreement no. 259349. The analysis presented in this paper is 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 Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).
Paper: 2016ApJ...827..127K (acknowledgments)
We thank Rodolfo Barniol Duran, Ehud Nakar, Re’em Sari, Elad Steinberg, and Almog Yalinewich for helpful discussions. J.K. and R.C. would like to thank the Hebrew University and its Institute for Advanced Studies for hospitality while the key ideas of this paper were developed. We are also grateful to Ehud Nakar for a loan of office space. This work was supported by the following grants: I-CORE 1829/12, ISA 3-10417 (T.P.); NSF AST-1028111 and AST-1516299, and NASA/ATP NNX14AB43G (J.K.).
Paper: 2015MNRAS.448.3314D (acknowledgments)
This research has been supported by the National Science Foundation under grants PHY 11-25915 and AST 11-09174. This project was also supported by JINA (NSF grant PHY 08-22648). FH and DV acknowledge funding from Natural Sciences and Engineering Research Council of Canada. PD is grateful to the staff of the Max-Planck-Institut für Astrophysik, where this project was completed, for their warm hospitality. We thank M. Salaris who has generously provided us with the Sbordone et al. bolometric corrections.
Paper: 2019MNRAS.487.2665B (acknowledgments)
ACKNOWLEDGEMENTS IB is supported by an Alexander von Humboldt postdoctoral fellowship. The authors are grateful for comments by the referee which greatly improved this manuscript. The algorithms were set up using matlab ® .
Paper: 2016ApJ...825...70D (acknowledgments)
F.D. and V.K. acknowledge support from grant NSF AST-1517753 and Northwestern University through the “Reach for the Stars” program. The authors also thank our colleagues Dimitri Veras, Jeremy Sepinsky, Michael Efroimsky, and Lorenzo Iorio who provided insight and expertise that greatly assisted the research. We are thankful for their comments that greatly improved the manuscript during its composition and revising stages.
Paper: 2018ApJ...865...10S (acknowledgments)
We thank Phil Armitage, Ilse Cleeves, Ilaria Pascucci, Richard Teague, and Upasana Das for useful discussions related to this work. We also thank the anonymous referee whose comments improved the quality of this paper. J.B.S. acknowledges support from NASA grants NNX13AI58G and NNX16AB42G, and from NSF grant AST 1313021. The computations were performed on Stampede , Stampede 2 , and Maverick through XSEDE grants TG-AST120062 and TG-AST140001. We thank the Kavli Institute for Theoretical Physics, supported in part by the National Science Foundation under Grant No. NSF PHY-1125915, for hospitality during the completion of the paper. Software: Athena (Stone et al. 2008 ).
Paper: 2016ApJ...833...28M (acknowledgments)
We would like to thank the late Prof. Janusz Gil for his leadership and inspiration, which have motivated us to start the MSPES project. We thank the referee for his comments, which helped to improve the paper. We thank Prof. Joanna Rankin and Dr. W. Lewandowski for critical comments on the manuscript. We would like to thank the staff of GMRT and NCRA for providing valuable support in carrying out this project. This work was supported by grants DEC-2012/05/B/ST9/03924 and DEC-2013/09/B/ST9/02177 of the Polish National Science Centre. This work has been supported by Polish National Science Centre grant DEC-2011/03/D/ST9/00656 (K.K.). This work was financed by the Netherlands Organisation for Scientific Research (NWO) under project ”CleanMachine” (614.001.301).
Paper: 2019MNRAS.490.1135N (acknowledgments)
ACKNOWLEDGEMENTS We thank Guillermo Barro for sharing Σ 1 values and Dale Kocevski for helpful advice. QN, GY, and WNB acknowledge support from Chandra X-ray Center grant GO8-19076X, NASA ADP grant 80NSSC18K0878, the V.M. Willaman Endowment, and Penn State ACIS Instrument Team Contract SV4-74018 (issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060). DMA thanks the Science and Technology Facilities Council (STFC) for support from grant ST/L00075X/1. BL acknowledges financial support from the National Key RD Program of China grant 2016YFA0400702 and National Natural Science Foundation of China grant 11673010. FV acknowledges financial support from CONICYT and CASSACA through the Fourth call for tenders of the CAS-CONICYT Fund. YQX acknowledges support from the 973 Program (2015CB857004), NSFC-11890693,NSFC-11421303, the CAS Frontier Science Key Research Program (QYZDJ-SSW-SLH006), andK.C. Wong Education Foundation. The Chandra Guaranteed Time Observations (GTO) for the GOODS-N were selected by the ACIS Instrument Principal Investigator, Gordon P. Garmire, currently of the Huntingdon Institute for X-ray Astronomy, LLC, which is under contract to the Smithsonian Astrophysical Observatory via Contract SV2-82024.
Paper: 2016MNRAS.462S.547R (acknowledgments)
Acknowledgments We thank the following institutions and agencies for support of this work: Italian Space Agency (ASI, Italy) contract number I/024/12/1, Centre National dtudes Spatiales (CNES, France), DLR (Germany), NASA (USA) Rosetta Program and Science and Technology Facilities Council (UK). The work of UF, LD and partially salary of GR was supported by NASA Rosetta Grant JPL-1270007. VIRTIS was built by a consortium, which includes Italy, France and Germany, under the scientific responsibility of the Istituto di Astrofisica e Planetologia Spaziali of INAF, Italy, which also guides the scientific operations. The VIRTIS instrument development, led by the prime contractor Leonardo-Finmeccanica (Florence, Italy), has been funded and managed by ASI, with contributions from the Observatoire de Meudon financed by CNES, and from DLR. We thank the Rosetta Science Ground Segment and the Rosetta Mission Operations Centre for their support throughout all the phases of the mission. The VIRTIS calibrated data will be available through the ESAs Planetary Science Archive Website ( www.rssd.esa.int/index.php?projectPSApageindex ) and is available upon request until posted to the archive.
Paper: 2018MNRAS.476..673T (acknowledgments)
Acknowledgements We thank Zoltán Haiman and Kazuyuki Sugimura for useful discussions. This work is partially supported by the Simons Foundation through the Simons Society of Fellows (KI) and by Japan Society for the Promotion of Science Grant-in-Aid for Scientific Research (A) (17H01102 KO), for Scientific Research (C) (15K05036 KO; 16K05309 KO and 17K05383 SM)) and for Young Scientists (17K14260 HRT). This research was also supported by the Ministry of Education, Culture, Sports, Science and Technology as ‘Priority Issue on Post-K computer’ (Elucidation of the Fundamental Laws and Evolution of the Universe) and the Joint Institute for Computational Fundamental Science. Numerical computations were carried out on Cray XC30 at Center for Computational Astrophysics, National Astronomical Observatory of Japan.
Paper: 2017MNRAS.471..355I (acknowledgments)
Acknowledgements This research has made use of data and software 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. It is additionally based on observations obtained with XMMNewton , an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. The research also made use of the Swift /BAT transient monitor results provided by the Swift /BAT team. We would like to thank all the proposers of the archival observations used in this work. We would also like to thank the anonymous referee for his/her suggestions, which helped improve the manuscript.
Paper: 2017ApJ...837..134Z (acknowledgments)
We wish to thank Dick Manchester and George Hobbs for helpful discussion and suggestions. Furthermore, we thank Hao Tong and Mingyu Ge for communication on the latest progress on the time delay measurements of the Crab Pulsar. This research is supported by the National Natural Science Foundation of China, under the grant NSFC11373018 and NSFC11503006. We are also thankful for the support of the grant Beyond the Horizons 2012, and the support of the Strategic Priority Research Program of the Chinese Academy of Sciences Grant No. XDB23010200.
Paper: 2019ApJ...880..122Z (acknowledgments)
This work is supported by the National Science Foundation of China (41731068, 41774175, and 41621063). The authors thank the FGM and CIS instrument teams of Cluster and the FGM and ESA instrument teams of THEMIS for providing data and the NASA/GSFC’s Space Physics Data Facility for the OMNIWeb service. The OMNI data are available at http://cdaweb.gsfc.nasa.gov/cgi-bin/eval1.cgi . The authors are especially grateful to Dr. Khurana K. Krishan of UCLA for his insightful and useful suggestions for this paper.
Paper: 2017MNRAS.470.3806N (acknowledgments)
Acknowledgements EN acknowledges the Polish National Science Center grant no. 2014/13/B/ST9/00902. Calculations have been carried out at the Wrocław Centre for Networking and Supercomputing ( http://www.wcss.pl ), grant No. 214. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 097.C-0277 and 097.D-0478.
Paper: 2018ApJ...861...69C (acknowledgments)
Comments from an anonymous referee spurred substantial revisions to this paper. This research was supported by NSERC of Canada.
Paper: 2018ApJ...857...44K (acknowledgments)
We would like to thank an anonymous referee for helpful suggestions that improved the paper. This work is supported by the National Science Foundation under Grant No. AST-1616632, by the NASA Astrophysics Theory Program, by the NASA Astrophysics Data Analysis Program, and by Fermi Guest Investigator Program. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Facility at NASA Ames Research Center and NASA Center for Climate Simulation (NCCS) at NASA Goddard Space Flight Center.
Paper: 2015MNRAS.454.3597D (acknowledgments)
We thank the anonymous referee for valuable comments which further improved the quality of the paper. This research work is financially supported by S N Bose National Centre for Basic Sciences under Department of Science and Technology, Govt. of India. This publication makes use of data from The UKIRT Infrared Deep Sky Survey or UKIDSS which is a next generation near-IR sky survey using the wide field camera (WFCAM) on the United Kingdom Infrared Telescope on Mauna Kea in Hawaii. We also use data from Two-micron All-Sky Survey (2MASS), which is a joint project of the University of Massachusetts and Infrared Processing and Analysis Center/California Institute of Technology, funded by National Aeronautics and Space Administration and the National Science Foundation. This paper uses data observations made with the Spitzer Space Telescope , which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The authors are thankful to the HTAC members and staff of HCT, operated by Indian Institute of Astrophysics (Bangalore); JTAC members and staff of 1.04 m Sampurnanand telescope operated by Aryabhatta Research Institute of Observational Sciences (Nainital).
Paper: 2017MNRAS.472.4910L (acknowledgments)
Acknowledgements SK and MJH are supported by STFC grant ST/M001008/1. SK acknowledges a Senior Research Fellowship from Worcester College Oxford. EKL acknowledges support from the UK's Science and Technology Facilities Council (grant number St/K502029/1).
Paper: 2016ApJ...817..144B (acknowledgments)
The Berger GRB group at Harvard is supported in part by the NSF under grant AST-1411763 and by NASA under grant NNX15AE50G. This paper is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE1144152. W.F. acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant number PF4-150121 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We thank Ragnhild Lunnan, Maria Drout, Josh Grindlay, and Avi Loeb for helpful discussions. The HST data presented here and the Swift /UVOT data used in this work 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. Based in part on observations obtained at the Gemini Observatory, acquired through the Gemini Science Archive, and processed using the Gemini IRAF package, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil) and Ministerio de Ciencia, Tecnologia e Innovación Productiva (Argentina). Based in part on data obtained from the ESO Science Archive Facility. This paper makes use of data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. Based in part on data collected at the Subaru Telescope and obtained from SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. We thank S.B. Cenko for providing Palomar 60 inch afterglow images for GRBs 060206 and 090618, T. Krühler and J. Greiner for providing GROND afterglow images for GRBs 080520, 081121, and 081109 and a WHT image for GRB 090113, D. Malesani for providing a TNG afterglow image for GRB 060605, D. A. Kann for providing a WHT afterglow image for GRB 060124, and D. Perley for providing a Keck telescope afterglow image of GRB 071010A and a Palomar 60 inch afterglow image of GRB 080607.
Paper: 2018MNRAS.474..847K (acknowledgments)
ACKNOWLEDGEMENTS This study was conducted within the Emmy Noether research group on ‘Accretion Flows and Feedback in Realistic Models of Massive Star Formation’ funded by the German Research Foundation under grant no. KU 2849/3-1. Additionally, the authors would like to thank the anonymous referee for comments which helped clarify the discussion found here.