adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017MNRAS.469.4985K (acknowledgments)
Acknowledgments This work has been supported by Narodowe Centrum Nauki through research projects DEC-2011/01/B/ST9/03183 (JN) and DEC-2013/10/E/ST9/00662 (OK, JN and AB). MP acknowledges support through grant PO 1508/1-2 of the Deutsche Forschungsgemeinschaft. The numerical experiment was possible through a 7 Mcore-hour allocation on the 2.399 PFlop Prometheus system at ACC Cyfronet AGH. Part of the numerical work was conducted on resources provided by the North-German Supercomputing Alliance (HLRN) under project bbp00003 and also at the Pleiades facility at the NASA Advanced Supercomputing (NAS).
Paper: 2017A&A...606A...5V (acknowledgments)
We thank the anonymous referee for the constructive comments that helped us to improve the manuscript and the vertical reconstruction procedure. This work was supported by RFBR grant 17-02-00644. The simulations were performed on the Vienna Scientific Cluster (VSC-2), on the Shared Hierarchical Academic Research Computing Network (SHARCNET), on the Atlantic Computational Excellence Network (ACEnet). This publication is supported by the Austrian Science Fund (FWF).
Paper: 2019MNRAS.488.3439S (acknowledgments)
ACKNOWLEDGEMENTS I acknowledge computing time awarded at CDAC National Param supercomputing facility, India, under the grant ‘Hydromagnetic-Turbulence-PR’ and the use of ‘Nova’ cluster at IIA. I also thank the Science and Engineering Research Board (SERB) of the Department of Science Technology (DST), Government of India, for support through research grant ECR/2017/001535. It is a pleasure to thank Kandaswamy Subramanian for insightful discussions on decaying (M)HD turbulence and for his comments on the manuscript. I also thank the anonymous referee for a timely and and constructive report that helped to improve the quality of the paper. The software used in this work was in part developed by the DOE NNSA-ASC OASCR Flash Center at the University of Chicago.
Paper: 2017MNRAS.472..254C (acknowledgments)
Acknowledgements We thank the anonymous referee for the helpful and constructive comments. The results presented in this paper expand one chapter of PC's PhD thesis. We thank Michael Brown, Casey Papovich, and Ray Sharples for their constructive feedback and suggestions. This work was performed on the gSTAR national facility at Swinburne University of Technology. gSTAR is funded by Swinburne and the Australian Governments Education Investment Fund. We thank the Swinburne supercomputing and Information Technology teams for their support. We would like to thank Bianca Maria Poggianti and Alessia Moretti for providing us with the latest versions of the WINGS catalogues. We also thank Boris Häußler for providing the latest up to date scripts for galaxy image simulations. We thank Julie B. Nantais for providing updated redshift catalogues for the cluster RDCS J1252.9−2927. We thank Yara Jaffé for providing suggestions and stimulating discussions on the use of the EDisCS and WINGS data. PC acknowledges the support provided by FONDECYT postdoctoral research grant no. 3160375, by a Swinburne Chancellor Research Scholarship and an AAO PhD Scholarship. WJC gratefully acknowledges the financial support of an Australian Research Council Discovery Project grant throughout the course of this work. RD gratefully acknowledges the support provided by the BASAL Center for Astrophysics and Associated Technologies (CATA), and by FONDECYT grant no. 1130528. The data in this paper were based in part on observations obtained at the ESO Paranal Observatory (ESO programme 084.A-0214). Based on observations obtained at the Gemini Observatory, 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), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). Based on observations made with the NASA/ESA Hubble Space Telescope , obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. These observations are associated with Program ID 12051. Based on data obtained from the ESO Science Archive Facility (Program ID 073.A-0737(A)). Part 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.
Paper: 2019MNRAS.487.2522M (acknowledgments)
ACKNOWLEDGEMENTS First of all, we want to acknowledge the comments and suggestions of our anonymous referee, who really helped to improve the content and understanding of the paper. G. Marton and this work was supported by the Hungarian National Research, Development and Innovation Office (NKFIH) grant PD-128360. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme under grant agreement no. 716155 (SACCRED) and from grant 2017-2.2.5-TÉT-FR-2017-00027. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia DPAC ( https://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 publication makes use of data products from the WISE , which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in AAS 143, 23. Many figures and analyses were done with the topcat software (Taylor 2005 ).
Paper: 2015ApJ...798...37Z (acknowledgments)
We thank SeyedAbdolreza Sadjadi and Renaud Papoular for helpful discussions. The fitting models were done using the NASA Ames Research Center PAH IR Spectroscopic Database and software, and we thank Christiaan Boersma for making these resources publicly available. This work was partially supported by the Research Grants Council of the Hong Kong Special Administrative Region, China (project No. HKU 7031/10P).
Paper: 2017A&A...601A..13W (acknowledgments)
Part of this work was supported by the Agencia Nacional de Promoción Científica y Tecnológica (ANPCyT) through the Programa de Modernización Tecnolǵica BID 1728/OC-AR, by the PIP 112-200801-00940 grant from CONICET (Argentina). Some simulations were run on IFLySiB’s Cluster, which is part of SNCAD-MinCyT, Argentina.
Paper: 2019MNRAS.484..850P (acknowledgments)
ACKNOWLEDGEMENTS The authors would like to thank the anonymous referee for their very helpful comments in assisting with the discussions in this paper. In addition, would like to thank Russet McMillan for her help taking images to create a master I -band fringe pattern for the ARCTIC imager. We would also like to thank Dr. Stacy McGaugh for discussions on LSB photometry, especially morphological classifications. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of astropy , a community-developed core python package for Astronomy (Astropy Collaboration 2013 , 2018 ). We acknowledge the usage of the HyperLeda data base ( http://leda.univ-lyon1.fr ).
Paper: 2015MNRAS.452....2K (acknowledgments)
DK thanks Norbert Werner for a useful discussion about the links between the observed emission-line gas and the large-scale X-ray properties of NGC 5813. DK also thanks Michele Cappellari and Richard McDermid for comments on an early version of the paper. Based on observations made with ESO telescopes at the La Silla Paranal Observatory under programme ID 60.A-9100(A). RB acknowledges support from the ERC advanced grant 339659-MUSICOS.
Paper: 2017ApJ...840...29H (acknowledgments)
We gratefully acknowledge support from NSF grants AST-0709356 (L.Y.H. and L.L.C.) and AST-1313150 (A.J.B.), as well as the John Simon Guggenheim Memorial Foundation and Trustees of the William F. Vilas Estate (A.J.B.). I.R.S. acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL (321334), and a Royal Society/Wolfson Merit Award. The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China and the Chinese Academy of Sciences (Grant No. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. The James Clerk Maxwell Telescope has historically been 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 the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We acknowledge the cultural significance that the summit of Maunakea has to the indigenous Hawaiian community.
Paper: 2019MNRAS.488.2006E (acknowledgments)
ACKNOWLEDGEMENTS DSE acknowledges the financial support of the Science and Technology Facilities Council through a studentship award. We would like to thank the anonymous referee for constructive comments that helped to improve this paper as well as Jose Oñorbe, Tilman Hartwig, Bhaskar Agarwal, and Marta Volonteri for their useful discussions and comments. This research made use of astropy , a community-developed core python package for Astronomy (Astropy Collaboration 2013 ).
Paper: 2017A&A...601A..57B (acknowledgments)
The authors wish to thank the CoRoT and Kepler Teams whose efforts made these results possible. The CoRoT space mission has been developed and was operated by CNES, with contributions from Austria, Belgium, Brazil, ESA (RSSD and Science Program), Germany, and Spain. Funding for Kepler ’s Discovery mission is provided by NASA’s Science Mission Directorate. S.B.F. wishes to thank E. Michel for encouraging him to study Scuti stars, and the Solar Physics Team of the Universitat de les Illes Balears (UIB) for hosting his stay in Majorca. He has received financial support from the Spanish Ministry of Science and Innovation (MICINN) under the grant AYA2010-20982-C02-02. A.G.H. acknowledges support from Fundação para a Ciência e a Tecnologia (FCT, Portugal) through the fellowship SFRH/BPD/80619/2011. R.A.G. acknowledges the financial support from the ANR (Agence Nationale de la Recherche, France) program IDEE (n ANR-12-BS05-0008) “Interaction Des Étoiles et des Exoplanètes” and from the CNES GOLF and PLATO grants at CEA.
Paper: 2019ApJ...878..125T (acknowledgments)
We would like to thank our referee, Ralph Schönrich, whose detailed and accurate comments much improved the presentation of our paper. T.T. also thanks Takuma Suda for his advice on practical use of the SAGA database. This work was supported by JSPS KAKENHI grant Nos. 18H01258, 18H04593, 16H04081, 18H01248, 17H02870, and 18K03711.
Paper: 2019MNRAS.490.4786G (acknowledgments)
ACKNOWLEDGEMENTS RG thanks Michael Fall for very useful discussions and comments on an earlier version of the manuscript, and the referee for providing a very constructive and useful report that led to the improvement of this paper. FvdV was supported by the Deutsche Forschungsgemeinschaft through project SP 709/5-1. JZ acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 679145, project ‘COSMO-SIMS’). FAG acknowledges financial support from CONICYT through the project FONDECYT Regular Nr. 1181264, and funding from the Max Planck Society through a Partner Group grant. FM is supported through the Program ‘Rita Levi Montalcini’ of the Italian MIUR.
Paper: 2016A&A...596A..39K (acknowledgments)
We are grateful to John Peacock for his useful comments. Special thanks to Mark Taylor for the TOPCAT 8 ( Taylor 2005 ) and STILTS 9 ( Taylor 2006 ) software. Some of the results in this paper have been derived using the HEALPix package 10 ( Górski et al. 2005 ). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. This research has made use of data obtained from the SuperCOSMOS Science 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. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. M.B., K.M., A.P., A.K. and M.K. were supported by the Polish National Science Center under contract #UMO-2012/07/D/ST9/02785. T.K., K.M. and A.P. were supported by the National Science Centre (grants UMO-2012/07/B/ST9/04425 and UMO-2013/09/D/ST9/04030), the Polish-Swiss Astro Project (co-financed by a grant from Switzerland, through the Swiss Contribution to the enlarged European Union), and the European Associated Laboratory Astrophysics Poland-France HECOLS. M.B. was supported by the Netherlands Organization for Scientific Research, NWO, through grant No. 614.001.451, and through FP7 grant No. 279396 from the European Research Council.
Paper: 2019A&A...631A.128C (acknowledgments)
We thank M. A. T. Groenewengen for the helpful comments. We acknowledge the support from the ERC Consolidator Grant funding scheme ( project STARKEY , G.A. n. 615604). A. B. acknowledges support from PRIN-MIUR 2017. T. S. R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli). For the plots we used matplotlib, a Python library for publication quality graphics ( Hunter 2007 ).
Paper: 2016MNRAS.459.1745F (acknowledgments)
Support for programme GO 11598 was provided by NASA through a grant from the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Much of the data presented herein were obtained at the W.M. Keck Observatory, which operates 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. Additionally, partial support for this work came from NASA ATP NNX12AH86G, HST grants HST-GO-11598 and HST-GO-12248, NASA ADP grant NNX08AJ44G, NSF grants AST-0847667 and AST-133514, and the South African National Research Foundation's Research Chairs programme. The simulations used here were run on computing facilities owned by the Carnegie Observatories. Computing resources used for this work were made possible by a grant from the Ahmanson foundation, and through grant DMS-0619881 from the National Science Foundation. Facilities : Keck: I (HIRES), Hubble (COS).
Paper: 2018MNRAS.475.4825T (acknowledgments)
Acknowledgements We would like to thank the anonymous referee for suggesting revisions that greatly improved the quality of the paper. We also thank Anatoly Klypin for insightful discussions, and Andrea Macciò and Aaron Dutton for generously providing their NIHAO data. AS acknowledges support from the Swiss National Science Foundation (PZ00P2_161363).
Paper: 2019ApJ...881..152K (acknowledgments)
We thank Xianyu Tan and Xi Zhang for helpful comments on an early draft of this manuscript and the anonymous referee for helpful comments that significantly improved the manuscript. T.D.K. and A.P.S. acknowledge support from the Technology and Research Initiative Fund (TRIF) at the University of Arizona. T.D.K. acknowledges funding from the 51 Pegasi b Fellowship in Planetary Astronomy sponsored by the Heising–Simons Foundation.
Paper: 2015ApJ...802...95R (acknowledgments)
We are grateful to N. Bucciantini, B. Metzger, T. Piran, and B. Zhang for useful discussions and comments. Support comes from the DFG Grant SFB/Transregio 7, from “NewCompStar,” COST Action MP1304, and from HIC for FAIR.
Paper: 2018MNRAS.481.5675Q (acknowledgments)
ACKNOWLEDGEMENTS We appreciate the help of the anonymous referee that, during the revision process, provided us comments and suggestions that allowed improving the manuscript. CQN acknowledges the support of the ISAS/JAXA International Top Young Fellowship and the JSPS KAKENHI grant number 18K13596. The sunrise -3 project is supported in Japan by the funding from ISAS/JAXA for the small-scale program for novel solar observations and the JSPS KAKENHI grant numbers 18H03723 and 18H05234. This research was supported by the Research Council of Norway through its Centres of Excellence scheme, project number 262622. This work has also been supported by Spanish Ministry of Economy and Competitiveness through the project ESP-2016-77548-C5-1-R. DOS also acknowledges financial support through the Ramón y Cajal fellowships.
Paper: 2017A&A...601A..10V (acknowledgments)
S.V.E. is FRS-FNRS Research Associate. P.N. is Boursier F.R.I.A. (FNRS, Belgium). B.P.’s research is partially funded by the CNRS Programme National de Physique Stellaire. Support from the Fondation ULB is acknowledged. Based on observations made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations obtained with the HERMES spectrograph, which is supported by the Fund for Scientific Research of Flanders (FWO), Belgium, the Research Council of K.U. Leuven, Belgium, the Fonds de la Recherche Scientifique (F.R.S.-FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland and the Thüringer Landessternwarte Tautenburg, Germany. This work was partly funded by an Action de recherche concertée (ARC) from the Direction générale de l’Enseignement non obligatoire et de la Recherche scientifique – Direction de la recherche scientifique – Communauté française de Belgique. We wish to thank the referee Ian Short for very helpful comments which improved this paper.
Paper: 2019ApJ...871....6Y (acknowledgments)
The authors thank Ming Sun for contribution to the early development of this project. H.Y.K.Y acknowledges support from NASA ATP (grant No. NNX17AK70G) and NSF grant AST 1713722. M.G. is supported by NASA through Einstein Postdoctoral Fellowship Award Number PF5-160137 issued by the Chandra X-ray Observatory Center, which is operated by the SAO for and on behalf of NASA under contract NAS8-03060. Support for this work was also provided by Chandra GO7-18121X. The simulations presented in this paper were performed on Pleiades , provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, as well as the Deepthought2 cluster supported by the Division of Information Technology at the University of Maryland College Park. FLASH was developed largely by the DOE-supported ASC/Alliances Center for Astrophysical Thermonuclear Flashes at University of Chicago. Data analysis presented in this paper was conducted with the publicly available yt visualization software (Turk et al. 2011 ). We are grateful to the yt development team and community for their support. We acknowledge the “Multiphase AGN Feeding Feedback” 8 8 www.sexten-cfa.eu/event/multiphase-agn-feeding-feedback workshop at Sexten CfA (Italy) for stimulating interactions that helped to improve this work.
Paper: 2015ApJ...815...25L (acknowledgments)
This work was supported by NASA grant NNX13AI34G.
Paper: 2019ApJ...883..170M (acknowledgments)
We thank the referee for valuable suggestions that helped to improve the paper. The project was partially supported by National Science Centre, Poland, grant No. 2017/26/A/ST9/00756 (Maestro 9) and MNiSW grant DIR/WK/2018/12. V.K. acknowledges Czech Science Foundation No. 17-16287S. We acknowledges P. Du, Y.-R. Li, and J.-M. Wang for the provided data and comments that improved the paper. We acknowledge M. Bentz, C. J. Grier, J. Kuraszkiewicz, A. del Olmo, M. Fausnaugh, J. Mejía-Restrepo, and Y. Shen for the extra information required for the development of this work.
Paper: 2019ApJ...884..104L (acknowledgments)
This study uses data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey ( http://califa.caha.es/ ), which is 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). This study also uses the 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.