adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017MNRAS.470..379S (acknowledgments)
Acknowledgments The authors would like to thank the reviewer Professor M. Peimbert for comments and corrections and for pointing out the possible blend of the λ4089.29 line with an Si iv line. The work of PJS was supported in part by the STFC (grant ST/J000892/1). The complete data generated in this work can be obtained in electronic format with full precision from the Centre de Données astronomiques de Strasbourg (CDS) data base (catalog VI/150). The fortran 77 data server is compiled and tested thoroughly using gfortran, f77 and Intel fortran compilers on Ubuntu 12.04 and Scientific Linux platforms. Representative sample results from all these compilers and on all those platforms are compared and found to be identical within the stated numerical accuracy.
Paper: 2017MNRAS.469.1559G (acknowledgments)
Acknowledgments We thank Emily Levesque for helpful conversations and V. Ashely Villar for access to their SN 2010da spectra. We are grateful to our anonymous referee for a thoughtful and constructive review. The supernova research of AVF’s group at U.C. Berkeley is supported by Gary Cynthia Bengier, the Richard Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation and NSF grant AST–1211916. Some of AVF’s work was completed at the Aspen Center for Physics, which is supported by NSF grant PHY-1066293; he thanks the Center for its hospitality during the black holes workshop in 2016 June and July. This research makes use of observations from the Las Cumbres Observatory (LCO) network and is supported by National Science Foundation (NSF) grant AST-1313484. This research is based in part on observations made at the W. M. Keck Observatory; we are grateful to the Keck staff for their assistance, and we extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration (NASA); it was made possible by the generous financial support of the W. M. Keck Foundation. We thank Daniel Perley and Brad Cenko for the use of, and assistance with, their Keck LRIS imaging and spectroscopy reduction pipeline. 5 We also thank WeiKang Zheng, Kelsey Clubb, Brad Tucker, Patrick Kelly and Isaac Shivvers for their assistance with the observations. 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 NASA. This work has made use of the Weizmann Interactive Supernova Data Repository (Yaron Gal-Yam 2012 ) at http://wiserep.weizmann.ac.il .
Paper: 2015MNRAS.452.2897P (acknowledgments)
The authors acknowledge useful discussions with G. Nelemans and M. Dan. We acknowledge an anonymous referee for suggestions that helped us to improve the presentation of our results. LP acknowledges support from the PRIN-INAF 2011 project ‘Multiple populations in Globular Clusters: their role in the Galaxy assembly’. AT acknowledges support from the PRIN-MIUR 2010-2011 project ‘The Obscure Universe and the Cosmic Evolution of Barions’. LRY acknowledges support by RFBR grants 14-02-00604, 15-02-04053 and Presidium of RAS program P-41. This research has made use of NASA's Astrophysics Data System.
Paper: 2015MNRAS.449L.113H (acknowledgments)
GH acknowledges discussions with A. Tokovinin and K. Hełminiak. We also thank the referee for her/his helpful comments. Support for this project is provided by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Científica Milenio through grant IC 210009, awarded to the Millennium Institute of Astrophysics; by Proyecto Basal PFB-06/2007; by Fondecyt grant #1141141; and by CONICYT Anillo grant ACT 1101.
Paper: 2016A&A...590A..36C (acknowledgments)
The authors would like to thank Annie Hughes for providing the CO(1–0) data and Akiko Kawamura for the CO(3–2) data. This research was made possible through the financial support of the Agence Nationale de la Recherche (ANR) through the programme SYMPATICO (Program Blanc Projet (NR-11-BS56-0023) and also through the EU FP7. SH acknowledges financial support from DFG programme HO 5475/2-1. PACS was developed by MPE (Germany); UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development was supported by BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE was developed by Cardiff University (UK); Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); SNSB (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development was supported by CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).
Paper: 2019MNRAS.486..639K (acknowledgments)
ACKNOWLEDGEMENTS MJI was supported by the Australian Research Council Future Fellowship (FT130100235). This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement CoG #683029). JHG gratefully acknowledges support from the Director’s Research Funds at the Space Telescope Science Institute. The manuscript was also substantially improved following helpful comments from an anonymous referee.
Paper: 2017ApJ...850..118S (acknowledgments)
This work was financially supported by the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (grant agreement No 646717, TUNNELCHEM). The authors also acknowledge support for CPU time by the state of Baden-Württemberg through bwHPC and the German Research Foundation (DFG) through grant no. INST 40/467-1 FUGG. Software: DL-FIND (Kästner et al. 2009 ), DL_POLY (Smith et al. 2002 ), Molpro version 2015.1 (Werner et al. 2012 ), NWCHEM 6.6 (Valiev et al. 2010 ).
Paper: 2017MNRAS.469.3396C (acknowledgments)
Acknowledgments The authors would like to thank Nuala McCullagh for helpful discussions relating to the evolution of the matter power spectrum, and Violeta Gonzalez-Perez for helpful discussions relating to the evaluation of the Limber equation, for both this work and C16 . WIC and CGL acknowledge financial support and fruitful discussions from the Munich Institute for Astro- and Particle Physics (MIAPP) DFG cluster of excellence ‘Origin and Structure of the Universe’ workshop entitled ‘The Star Formation History of the Universe’, held in Munich in 2015 August. This work was supported by the Science and Technology Facilities Council [ST/K501979/1, ST/L00075X/1]. CMB acknowledges the receipt of a Leverhulme Trust Research Fellowship. This work 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 ). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.
Paper: 2017MNRAS.469.2313G (acknowledgments)
Acknowledgments This work is supported by the Scientific and Technological Research Council of Turkey (TBTAK) under the grant 113F354. Preliminary results of this paper were presented at NewCompStar 2015 Annual Meeting held in Budapest, Hungary, which was supported by COST action MP1304. I am grateful to M. Ali Alpar for fruitful discussions on this and related topics over the years. I wish to express my special thanks to Peter S. Shternin for useful remarks on the cooling of neutron stars. I acknowledge the referee for insightful comments that lead to clarification of some points.
Paper: 2016MNRAS.462S.507H (acknowledgments)
Acknowledgments We thank Daniel Bardin for his help with the Observatoire de Haute Provence (OHP, France) observations; OHP, IUCAA Observatory (India) and Chandra Himalayan telescope (India) for attribution of observing time; and Programme National de Plantologie (PNP, France) for support. This work was partly supported by CNES, in relation to observations of MIDAS on the Rosetta mission and to measurements with PROGRA2 instruments on parabolic flights on A300-ZeroG. Support for HST comet observations in program numbers GO13863 and 144261 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 Incorporated, under NAS5-26555.
Paper: 2017A&A...603A..80M (acknowledgments)
The authors are very thankful to the referee for valuable comments that helped to improve the paper. The authors would also like to thank Jesper Rasmussen and Alastair Sanderson for kindly providing their observational data, as well as Susana Planelles and Elena Rasia for kindly providing their simulation outputs and for useful discussions. This work is partly based on the XMM-Newton AO-12 proposal “The XMM-Newton view of chemical enrichment in bright galaxy clusters and groups” (PI: de Plaa), and is a part of the CHEERS (CHEmical Evolution Rgs cluster Sample) collaboration. H.A. acknowledges the support of NWO via a Veni grant. P.K. acknowledges financial support from STFC. C.P. acknowledges support from ERC Advanced Grant Feedback 340442. T.H.R. acknowledges support from the DFG through grant RE 1462/6 and through the Transregional Collaborative Research Centre TRR33 The Dark Universe, project B18. This project has been supported by the Lendület LP2016-11 grant awarded by the Hungarian Academy of Sciences. This work is based on observations obtained with XMM-Newton , an ESA science mission with instruments and contributions directly funded by ESA member states and the USA (NASA). The SRON Netherlands Institute for Space Research is supported financially by NWO, The Netherlands Organisation for Scientific Research.
Paper: 2019ApJ...874..115B (acknowledgments)
The authors thank I. Cooke, R. Martin-Domenech, P. Maksiutenko, and L. Kelley for valuable feedback. J.B.B. acknowledges funding from the National Science Foundation Graduate Research Fellowship under grant DGE1144152. This work was supported by an award from the Simons Foundation (SCOL # 321183, K.O.). Software: NumPy (Van Der Walt et al. 2011 ), Matplotlib (Hunter 2007 ), emcee (Foreman-Mackey et al. 2013 ).
Paper: 2017A&A...599A.132L (acknowledgments)
We kindly thank Jun Li and Hua Guo for providing the potential energy surface. Astrochemistry in Leiden in general was supported by the European Community’s Seventh Framework Programme (FP7/2007–2013) under grant agreement No. 238258, the Netherlands Research School for Astronomy (NOVA) and from the Netherlands Organization for Scientific Research (NWO) within the framework of the Dutch Astrochemistry Network. SI acknowledges the Royal Society for financial support. T.L. was supported by the Dutch Astrochemistry Network financed by NWO. T.L. and J.K. were financially supported by the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 646717, TUNNELCHEM).
Paper: 2016ApJ...826..190A (acknowledgments)
This work was supported by the 973 program (2013CB837900), National Science Foundation of China (U1331205). W.A.B. has been supported as a Visiting Professor of the Chinese Academy of Sciences (KJZD-EW-T01). P.M. thanks the support through the CAS PIFI program. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The e-MERLIN is a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of the UK Science and Technology Facilities Council (STFC). This research has made use of the United States Naval Observatory (USNO) Radio Reference Frame Image Database (RRFID). This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009a ).
Paper: 2017MNRAS.464...65P (acknowledgments)
SPCP is grateful to the Space Telescope Science Institute, Baltimore, USA, the Research School for Astronomy and Astrophysics, Australian National University, Canberra, Australia, and the Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain, for hospitality and support during short and extended working visits in the course of his PhD thesis research. He thanks Roelof de Jong and Ron Allen for help and support during an earlier period as a visiting student at Johns Hopkins University and the Physics and Astronomy Department, Krieger School of Arts and Sciences for this appointment. PCK thanks the directors of these same institutions and his local hosts Ron Allen, Ken Freeman and Johan Knapen for hospitality and support during many work visits over the years, most of which were directly or indirectly related to the research presented in this series of papers. Work visits by SPCP and PCK were supported by an annual grant from the Faculty of Mathematics and Natural Sciences of the University of Groningen to PCK, accompanying his distinguished Jacobus C. Kapteyn professorship, and by the Leids Kerkhoven-Bosscha Fonds. PCK's work visits were also supported by an annual grant from the Area of Exact Sciences of the Netherlands Organization for Scientific Research (NWO), in compensation for his membership of its board.
Paper: 2017MNRAS.472.2926L (acknowledgments)
Acknowledgements We are very grateful to the anonymous referee for his/her very valuable comments. This work is partially supported by the National Natural Science Foundation of China (NSFC 11433004 and 11173020), Top Talents Program of Yunnan Province, the Natural Science Foundation of Yunnan Province (2013FB063), the Young Teachers Program of Yuxi Normal University, and the Program for Innovative Research Team (in Science and Technology) in University of Yunnan Province (IRTSTYN).
Paper: 2019A&A...624A.135Y (acknowledgments)
We made use of observations from the AIA and HMI instruments on board the SDO mission (available at jsoc.stanford.edu ), the SILSO sunspot number record ( www.sidc.be/silso/ ), and the IUP Mg II index composite ( www.iup.uni-bremen.de/gome/gomemgii.html ). This study was supported by the German Federal Ministry of Education and Research under project 01LG1209A.
Paper: 2016MNRAS.456...55G (acknowledgments)
We thank the anonymous referees for carefully reading the manuscript and for valuable comments that helped improve this paper substantially. We also thank Professor Yang Chen for discussions, Dr Rai Yuen for smoothing out the language and Dr Cristobal Espinoza for useful suggestions on the braking indices of several radio pulsars. This work was supported by Xinjiang Natural Science Foundation No. 2013211A053, by Chinese National Science Foundation through grants Nos 11173041, 11173042, 11273051, 11373006 and 11133001, by the National Basic Research Programme of China grants 973 Programmes 2012CB821801, by the Strategic Priority Research Programme ‘The Emergence of Cosmological Structures’ of the Chinese Academy of Sciences through No. XDB09000000 and by the West Light Foundation of Chinese Academy of Sciences No. 2172201302.
Paper: 2019ApJ...871...38K (acknowledgments)
This work was supported by NASA ATP Grant NNX14AP92G and NSF Grant AST-1716762. K.K. acknowledges support by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1324585. S.C. acknowledges support from CIERA, the National Aeronautics and Space Administration through a Chandra Award Number TM5-16004X/NAS8-03060 issued by the Chandra X-ray Observatory Center (operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060), and Hubble Space Telescope Archival research grant HST -AR-14555.001-A (from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555).
Paper: 2019MNRAS.484.5755O (acknowledgments)
ACKNOWLEDGEMENTS We acknowledge the ‘Accordo Quadro INAF-CINECA (2017)' for the availability of high performance computing resources and support. Simulations have been performed as part of the class-A project ‘Three-dimensional relativistic simulations of bow shock nebulae' (PI B. Olmi). The authors also acknowledge financial support from the PRIN-MIUR project prot. 2015L5EE2Y ‘Multi-scale simulations of high-energy astrophysical plasmas'. B. Olmi wishes also to acknowledge Andrea Mignone, from the PLUTO team, for fundamental support, and Simone Landi and Luca Del Zanna for fruitful discussions.
Paper: 2015ApJ...812...26D (acknowledgments)
We thank the anonymous referee for a constructive and helpful report, E. Schunová for her feedback on earlier versions of this manuscript, S. D. Miller for comments on his results, and P. Wiegert for sharing the details of his pre-impact orbital solution. This work was partially supported by the Spanish “Comunidad de Madrid” under grant CAM S2009/ESP-1496. Some of the calculations discussed here were completed on the “Servidor Central de Cálculo” of the Universidad Complutense de Madrid. In the preparation of this paper, we made use of the NASA Astrophysics Data System, the ASTRO-PH e-print server, the MPC data server, and the NEODyS information service.
Paper: 2019ApJ...882....5W (acknowledgments)
We are grateful to Dr. J.M.D. Kruijssen and the organizers of the conference “The Multi-Scale Physics of Star Formation and Feedback during Galaxy Formation” in Heidelberg, 2018 June, for providing a collaborative atmosphere where two of the authors, B.G.E. and C.D.W., began discussing this project. We also acknowledge useful comments by the referee. C.D.W. acknowledges financial support from the Canada Council for the Arts through a Killam Research Fellowship. The research of C.D.W. is supported by grants from the Natural Sciences and Engineering Research Council of Canada and the Canada Research Chairs program. A.B. wishes to acknowledge partial support from an Ontario Trillium Scholarship (OTS). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00525.S, ADS/JAO.ALMA#2012.1.00165.S, ADS/JAO.ALMA#2013.1.00218.S, ADS/JAO.ALMA#2013.1.00379.S, ADS/JAO.ALMA#2015.1.00167.S,ADS/JAO.ALMA#2015.1.00287.S, ADS/JAO.ALMA#2015.1.00993.S, ADS/JAO.ALMA#2016.1.00140.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. 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 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. Facility: ALMA. Software: astropy (Astropy Collaboration et al. 2013 ), CASA (McMullin et al. 2007 ).
Paper: 2016A&A...592A..79N (acknowledgments)
The authors are very grateful to the referee, Frans Snik, for his insightful suggestions and helpful comments to improve the quality of the original manuscript. This work is partially supported by the National Aeronautics and Space Administration under Grants NNX12AG05G and NNX14AD33G issued through the Astrophysics Research and Analysis (APRA) program (PI: R. Soummer). M.N. would like to thank Rémi Soummer and Laurent Pueyo for their support. M.N. would also like to acknowledge the ESO Chile Visiting Scientist program. Finally, A.V. would like to thank the Paranal staff for their patience and support when performing the tests presented in this work. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF Osservatorio di Padova (Italy), Observatoire de Genève (Switzerland), ETH Zurich (Switzerland), NOVA (Netherlands), ONERA (France) and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (20042008), grant number 226604 for FP7 (20092012) and grant number 312430 for FP7 (20132016).
Paper: 2015A&A...576A.136M (acknowledgments)
We thank Stephen White who edited the GMRT data of April 06, 2006 when he was a visiting scientist in Meudon in July 2006. P. Subramanian acknowledges partial support from the CAWES-II program, administrated by the Indian Space Research Organization. We also thank N. G. Kantharia and S. Ananthakrishnan for helpful discussions regarding GMRT observation procedures, and an anonymous referee for helping us to improve the manuscript.
Paper: 2017MNRAS.469.4999D (acknowledgments)
Acknowledgments We are grateful to Dr D. Weisz, Dr A. McConnachie and Dr N. Ho and collaborators for generously providing their data for this project. The authors thank the anonymous referee for the comments that have helped to improve this paper. AdP also thanks S. Bertran de Lis for her support and help during this project. This research was supported by the Polish National Science Centre under grant 2013/10/A/ST9/00023.
Paper: 2016ApJ...824...29S (acknowledgments)
We thank Mark Reid for pointing out the large amount of high-mass clumps that would be required to account for the global Galactic HCN and IR luminosities. This work was supported by NASA grant NNX12AE42G and NSF grant AST-1211844. A.E.G. acknowledges support from FONDECYT grant 3150570. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com .
Paper: 2018MNRAS.476.5127R (acknowledgments)
ACKNOWLEDGEMENTS The authors thank Adrick Broeils, Martha P. Haynes, J. M. van der Hulst, and Marc A. W. Verheijen, as well as the THINGS, LITTLE THINGS, and WHISP collaborations, for providing H i data cubes and moment maps of archival data. The authors also acknowledge the referee for their insight and helpful recommendations that improved this manuscript. This paper is based on work presented in EER's PhD dissertation, which was accepted by Indiana University graduate faculty in partial fulfilment of the requirements for the degree. The authors acknowledge observational and technical support from the National Radio Astronomy Observatory (NRAO). We acknowledge use of the WIYN 0.9 m telescope operated by WIYN Inc. on behalf of a Consortium of ten partner Universities and Organizations, and the WIYN 3.5 m telescope. The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, the National Optical Astronomy Observatory, and the University of Missouri. This work is based 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. E.E.R. acknowledges support from the Provost's Travel Award for Women in Science, a professional development fund supported through the Office of the Provost at Indiana University Bloomington, the Indiana University College of Arts and Sciences Dissertation Year Fellowship, and the Indiana Space Grant Consortium. L.v.Z. recognizes support from the Helena Kluyver Female Visitor programme at ASTRON during which some of this analysis was completed. This work was partially supported by NASA ADAP award NNX17AF17G. This research has made use of the NASA/IPAC Extragalactic Database (NED) that is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.