adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017A&A...597A..17H (acknowledgments)
This project has been funded by the BBVA Foundation under the Convocatoria 2015 de Ayudas Fundación BBVA a Investigadores y Creadores Culturales. We thank E. Vázquez-Semadeni and J. Alves for very useful comments, and R. Lorente and I.Yamamura for their help with the AKARI data. We are indebted to the Calar Alto Observatory staff for their excellent work taking the near-IR data under the Service Mode program. NH thanks the ALMA Science Center in Santiago for hosting her during 2.5 months. I.d.G. acknowledges support fromMICINN (Spain) AYA2011-30228-C03 grant (including FEDER funds). A.P. and L.Z. acknowledge the financial support from UNAM-DGAPA-PAPITT IA102815 grant (México). D.B. has been funded by Spanish grant AYA2012-38897-C02-01. H.B. is funded by the Ramón y Cajal fellowship program number RYC-2009-04497. A.B. acknowledges financial support from the Proyecto Fondecyt de Iniciación 11140572, and scientific support from the Millenium Science Initiative, Chilean Ministry of Economy, Nucleus RC130007. M.T.R. acknowledges partial support from CATA (PB06, CONICYT-Chile). C.E. is partly supported by Spanish Grant AYA 2014-55840-P. 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, funded by the National Aeronautics and Space Administration.
Paper: 2017A&A...605A.114M (acknowledgments)
Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. All the figures presented here were made using Matplotlib ( Hunter 2007 ).
Paper: 2019MNRAS.484.2514C (acknowledgments)
ACKNOWLEDGEMENTS The authors are glad to thank the referee, Andrej Prša, for his valuable comments and recommendations that helped improve this work. B-CO would like to thank Kyle Conroy for his support with technical details in the implementation of phoebe .
Paper: 2019ApJ...880...98I (acknowledgments)
The imaging data used in this work was provided courtesy of the NASA/ SDO and the AIA and HMI science teams. The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at https://omniweb.gsfc.nasa.gov . The authors thank the Helioviewer project for providing easy browsing access to many solar imaging data sets. The authors are also grateful to the anonymous referee for numerous helpful comments that improved the final paper.
Paper: 2017ApJ...839....1L (acknowledgments)
We thank the anonymous referee for a constructive review. We thank Simon Radford and William Tan for help with the CSO observation and data reduction, and Junhao Liu for helpful discussions on RADEX modeling. X.L. acknowledges the support of a Smithsonian Predoctoral Fellowship and the program A for outstanding PhD candidate of Nanjing University. J.M.D.K. gratefully acknowledges support in the form of an Emmy Noether Research Group from the Deutsche Forschungsgemeinschaft (DFG), grant number KR4801/1-1. C.B. is supported by the National Science Foundation under Award No. 1602583. Z.Y.Z. acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, cosmicism . We acknowledge the support by the National Natural Science Foundation of China (grant No. 11629302). This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013 ), and NASA’s Astrophysics Data System. This material is based upon work at the Caltech Submillimeter Observatory, which was operated by the California Institute of Technology. This publication is also based on data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. Facilities: SMA , VLA , CSO , APEX , GBT . Software: CASA, MIRIAD, MIR, GILDAS/CLASS, Astropy (Astropy Collaboration et al. 2013 ), RADEX (van der Tak et al. 2007 ), myRadex, correl_images.pro.
Paper: 2015A&A...584A...4D (acknowledgments)
P.D. thanks Philippe Laurent for his help in calculating elliptical integral numerical values. This research has made use of TOPCAT ( Taylor (2005) , http://www.starlink.ac.uk/topcat/ ) and SAOImage/DS9, developed by the Smithsonian Astrophysical Observatory ( http://hea-www.harvard.edu/RD/ds9/ ). This work profits from data downloaded from the SIMBAD database, operated at the CDS, and the VizieR catalogue access tool (CDS, Strasbourg, France; Ochsenbein et al. 2000 ). SPIRE was developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). PACS was developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). T.H. was supported by a CEA/Marie-Curie Eurotalents Fellowship. Part of this work was supported by the ANR (Agence Nationale pour la Recherche) project “PROBeS”, number ANR-08-BLAN-0241.
Paper: 2018MNRAS.475.2955L (acknowledgments)
Acknowledgements We thank the anonymous referee for valuable comments and suggestions that helped to significantly increase the quality of this work.
Paper: 2017MNRAS.469...13S (acknowledgments)
Acknowledgments We thank Mikoaj Jerzykiewicz for carefully reading the manuscript and language corrections. This work was financially supported by the Polish National Science Centre (grant 2015/17/B/ST9/02082). The calculations were carried out using resources provided by the Wrocaw Centre for Networking and Supercomputing ( http://wcss.pl ; grant 265).
Paper: 2016MNRAS.460.1658D (acknowledgments)
This work is a part of the project 176002 ‘Influence of collisional processes on astrophysical plasma line shapes’ supported by the Ministry of Education, Science and Technological Development of Serbia. It is also the result of Short term Scientific Mission CM0805 within COST programme on The Chemical Cosmos: Understanding Chemistry in Astronomical Environments. Partial financial support from project No 6572-20 Technical University – Sofia within Euroatom Programme is also acknowledged. This work has been supported as well, by the Paris Observatory, the CNRS and the PNPS (Programme National de Physique Stellaire, INSU-CNRS).
Paper: 2016MNRAS.457.3115S (acknowledgments)
This work has been financially supported by the Centre National d’Études Spatiales (CNES), the Institut National des Sciences de l'Univers (INSU), Airbus Group, Thales Alenia Space and the Région Limousin. We gratefully acknowledge Wolfgang Sohler for many helpful and stimulating discussions. Our thanks go also to A. Dexet for the development and his advices for all the specific mechanical components.
Paper: 2017ApJ...836...58M (acknowledgments)
We would like to thank the Department of Physics and Astronomy at BYU and the Departments of Physics at BYUI and UVU for support throughout this research. We are indebted to Kristin Chiboucas for many patient explanations of GMOS observing and to John Salzer for a helpful discussion. This report is 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, Tecnologa e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovaçäo (Brazil), for program GN-2015B-FT-15. This research is also based on observations at Kitt Peak National Observatory, National Optical Astronomy Observatory (NOAO Prop. ID: 2013A-0106; PI: J.W. Moody), which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. The authors are honored to be permitted to conduct astronomical research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham. Facilities: Mayall (MOSAIC-1.1 wide-field camera) , Gemini:Gillett (GMOS).
Paper: 2017A&A...603A..44N (acknowledgments)
F.W. is supported by the National Science Foundation (USA) under Grant PHY-1411708. S.S. acknowledges access to the computer facilities of the CSC Frankfurt. R.N. acknowledges financial support from the CAPES and CNPq.
Paper: 2016MNRAS.455L...1W (acknowledgments)
We thank the anonymous referee for constructive comments and suggestions. This work is supported by the NSFC (grants 11103003, 11133005, 11573009 and U1431124), National Basic Research Program of China (973 Program, No. 2014CB8455800), and New Century Excellent Talents in University (NCET-13-0238).
Paper: 2015ApJ...810...38K (acknowledgments)
We are grateful to the referee’s constructive comments. BBSO operation is supported by NJIT, US NSF AGS-1250818, NASA NNX13AG14G, AFOSR-FA9950-15-1-0322, and NST operation is partly supported by the Korea Astronomy and Space Science Institute and Seoul National University, and by stategic priority research program of CAS with Grant No. XDB09000000. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. The SDO data were (partly) provided by the Korea Data Center (KDC) for SDO in cooperation with NASA and SDO /HMI Team, which is operated by the Korea Astronomy and Space Science Institute. This work was conducted as a part of the effort of NASA’s Living with a Star Focused Team “Jets” funded by NASA LWS NNX11A073G grant. V. Yu also acknowledges support from AFOSR FA9550-12-0066 and NSF AGS-1146896 grants and the Korea Astronomy and Space Science Institute. This work was supported by a grant from the U.S. Air Force Research Laboratory, under agreement number FA 2386-14-1-4078 and by the planetary system research for space exploration from KASI. This work was also supported by the Maintenance of Korean Space Weather Center, a project of KASI, and the KASI basic research fund.
Paper: 2016A&A...590A.112M (acknowledgments)
This paper is based on observations collected with the 2.2 m telescope at the Centro Astronómico Hispano Alemán (CAHA) in Calar Alto (Spain) and the publicly available data obtained with the NASA space satellite Kepler . Operations at the Calar Alto telescopes are jointly performed by the Max-Planck-Institut für Astronomie (MPIA) and the Instituto de Astrofísica de Andalucía (CSIC). This research was partially funded by Spanish grant AYA2012-38897-C02-01. J.L.-B. thanks the CSIC JAE-predoc programme for Ph.D. fellowship support. R.B. is supported by CONICYT-PCHA/Doctorado Nacional. R.B. acknowledges additional support from project IC120009 “Millenium Institute of Astrophysics (MAS)” of the Millennium Science Initiative, Chilean Ministry of Economy. We wish to thank Ennio Poretti for very helpful comments. We acknowledge the use of the following internet-based resources: the ESO Digitized Sky Survey; the TEPCat catalogue; the SIMBAD database operated at CDS, Strasbourg, France; and the arXiv scientific paper preprint service operated by Cornell University.
Paper: 2017ApJ...846...71L (acknowledgments)
We thank the anonymous referee for a thoughtful and constructive report. This work is based on observations carried out with the IRAM NOEMA Interferometer and the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). This work was carried out as part of the PHANGS collaboration (formerly SFNG) and the PAWS collaboration. The work of A.K.L., M.G., and J.S. is partially supported by the National Science Foundation under Grant Nos. 1615105, 1615109, and 1653300. E.S. acknowledge financial support to the DAGAL network from the People Programme (Marie Curie Actions) of the European Union’s Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313. E.S. acknowledges funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (grant agreement No. 694343). A.H. acknowledges support from the Centre National d’Etudes Spatiales (CNES). J.M.D.K. and M.C. gratefully acknowledge financial support in the form of an Emmy Noether Research Group from the Deutsche Forschungsgemeinschaft (DFG), grant number KR4801/1-1 (PI: Kruijssen). J.M.D.K. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement number 714907, PI Kruijssen). G.B. is supported by CONICYT/FONDECYT, Programa de Iniciacion, Folio 11150220. A.U. acknowledges support from Spanish MINECO grants AYA2012-32295 and FIS2012-32096. F.B. ac- knowledges support from DFG grant BI1546/1-1. S.G.B. thanks economic support from grants ESP2015-68964-P and AYA2016-76682-C3-2-P.
Paper: 2019A&A...628A.100D (acknowledgments)
We thank the anonymous referee for the insightful comments. EC and RS acknowledges partial support from the Russian Science Foundation grant 19-12-00369. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00760.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. Basic research in radio astronomy at the US Naval Research Laboratory is funded by 6.1 Base funding, supporting T. Clarke. The scientific results reported in this article are obtained using the following softwares: AstroPy , a community-developed core Python package for Astronomy ( Astropy Collaboration et al. 2018 ); dynesty ( Speagle 2019 ); galario ( Tazzari et al. 2018 ).
Paper: 2016MNRAS.455.3381S (acknowledgments)
The authors are particularly grateful to Mohsen Shadmehri, De-Fu Bu and Richard Lovelace for their help and useful suggestions. We also appreciate the thoughtful and constructive comments of the referees, which clarified some points in the early version of the article. S. Abbassi acknowledges support from the International Center for Theoretical Physics (ICTP) for a visit through the regular associateship scheme. This work was supported by the Ferdowsi University of Mashhad under the grant 2/29823 (1393/1/19).
Paper: 2018MNRAS.481..639J (acknowledgments)
ACKNOWLEDGEMENTS J.J. acknowledges support by the Cambridge Trust and the Chinese Scholarship Council Joint Scholarship Programme (201604100032). D.J.W. acknowledges support from an Science and Technology Facilities Council Ernest Rutherford fellowship. M.L.P. is supported by a European Space Agency (ESA) research fellowship. A.C.F. acknowledges support by the European Research Council Advanced Grant 340442. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA, and data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This research has made use of the NuSTAR Data Analysis Software ( nustardas ) jointly developed by the ASI Science Data Center and the California Institute of Technology.
Paper: 2015A&A...578L...6B (acknowledgments)
We acknowledge the SVT team at ESO HQ for their help during the preparation of the OBs and the VLT team for conducting the observations. We thank C. P. Dullemond, G. Lesur, M. Min, and M. Tauras for fruitful discussions, and the referee for providing useful comments. M.B. acknowledges financial support from “Programme National de Physique Stellaire” (PNPS) of CNRS/INSU, France. C.G. was supported under the NASA Origins of Solar Systems program on NNG13PB64P. T.B. acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G.
Paper: 2019ApJ...872..193L (acknowledgments)
The NANOGrav Project receives support from NSF Physics Frontiers Center award number 1430284. Pulsar research at UBC is supported by an NSERC Discovery Grant and by the Canadian Institute for Advanced Research. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the NSF (AST-1100968) and in alliance with Ana G. Méndez-Universidad Metropolitana and the Universities Space Research Association. The National Radio Astronomy Observatory and the Green Bank Observatory are facilities of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. W.W.Z. is supported by the CAS Pioneer Hundred Talents Program and the Strategic Priority Research Program of the Chinese Academy of Sciences, grant No. XDB23000000. Author Contributions. M.T.L. developed the mathematical framework for this work, created the modified set of profiles and short-term residuals, performed the analysis, and prepared the majority of the manuscript. M.A.M. assisted with the preparation of the manuscript. All authors performed observations and/or helped produce the initial pulse-profile data set. Additional specific contributions will be described in the future NANOGrav 12.5 yr data set paper. Software: PSRCHIVE (Hotan et al. 2004 ; van Straten et al. 2012 ), nanopipe (Demorest 2018 ), PyPulse (Lam 2017 ).
Paper: 2016MNRAS.463.2849A (acknowledgments)
We are grateful to M. Mori, K. Yoshikawa, A. Y. Wagner, A. Burkert, F. Nakamura, H. Yajima, and A. Inoue for fruitful discussion. The numerical simulations have been performed with coma provided by Interdisciplinary Computational Science Program in Center for Computational Sciences, University of Tsukuba, and with cray xc30 at Center for Computational Astrophysics, NAOJ. This research was supported in part by Grant-in-Aid for Scientific Research (B) by JSPS (15H03638) (MU) and a grant from NAOJ (KH).
Paper: 2016MNRAS.459..673N (acknowledgments)
RCN acknowledges the financial support from CAPES Scholarship Box 13222/13-9. SP acknowledges the Department of Atomic Energy (DAE), Govt. of India, for a Post-Doctoral grant (File No. 2/40(60)/2015/RD-II/15420). SP also acknowledges the Department of Mathematics, Jadavpur University, where the work was initiated and some of the parts were carried out. The authors are very grateful to Diego Pavón for his useful comments. The authors are also very grateful to the anonymous referee for many illuminating comments which improved the manuscript considerably. Lastly, we must acknowledge the assistant editor for pointing out some setting problems in the figures.
Paper: 2015MNRAS.446.2629E (acknowledgments)
We thank the anonymous referee for helpful comments that improved the presentation of the work. We also thank Mauro Sereno, Marco De Petris and Dominique Eckert for discussion and comments on the manuscript. We acknowledge the financial contribution from contracts ASI-INAF I/009/10/0 and PRIN-INAF 2012.
Paper: 2018MNRAS.477.2419M (acknowledgments)
ACKNOWLEDGEMENTS We thank the anonymous referee for insightful comments. We acknowledge support from NSF AST 16-15688, the NASA/NY Space Grant fellowship, and contributions made by The Marvin Clan, Babette Josephs, Manit Limlamai, and the 2015 Crowd Funding Campaign to Support Milky Way Research. JLC acknowledges support from AST 11-51462. TCB acknowledges partial support for this work from grant PHY 14-30152; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation. PD acknowledges partial funding from a Natural Sciences and Engineering Research Council of Canada grant to D. VandenBerg. 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 Website is http://www.sdss3.org/ .
Paper: 2015MNRAS.446.4019B (acknowledgments)
The Parkes Observatory is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We thank the reviewer, Dipankar Bhattacharya, for suggestions which helped improve the manuscript.
Paper: 2018ApJ...868...11L (acknowledgments)
This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). We acknowledge the use of public data from the Swift data archive. This research is also based on observations obtained with XMM-Newton , an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. It has made use of data and/or 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. We appreciate constructive advice and comments by the referee. A.C.F. acknowledges ERC Advanced Grant 340442. S.T. and A.C.L. are supported by NASA grant NNX16AF82G. Facilities: Suzaku , Swift , XMM-Newton . Software: SAS, HEASoft.
Paper: 2019MNRAS.489.1697M (acknowledgments)
ACKNOWLEDGEMENTS This paper was based on the observation data collected at OHP Observatory, France. TM, TG, MP, and FKT are grateful for the support from the Swiss National Science Foundation, project SCOPES No. IZ73Z0152485. MP acknowledges significant support to NuGrid from NSF grant PHY-1430152 (JINA Center for the Evolution of the Elements) and STFC (through the University of Hull’s Consolidated Grant ST/R000840/1), and access to viper , the University of Hull High Performance Computing Facility. MP acknowledges the support from the ‘Lendlet-2014’ Programme of the Hungarian Academy of Sciences(Hungary), and from the BRIDGCE UK network. FKT acknowledges support from the European Research Council (FP7) under ERC Advanced Grant Agreement 321263 FISH. BC and MP acknowledges support from the ERC Consolidator Grant(Hungary) funding scheme (project RADIOSTAR, G.A. n. 724560) and from the National Science Foundation (USA) under grant No. PHY-1430152 (JINA Center for the Evolution of the Elements). This article is based upon work from the ChETEC COST Action (CA16117), supported by COST (European Cooperation in Science and Technology). TM thanks to S. Korotin for discussions. The authors appreciate very useful comments provided by the anonymous referee.