adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017A&A...602A..42K (acknowledgments)
We thank the staff at the JAO and the EU ARC Network who have participated in the EOC and Science Verification activities, observations and data reduction that made the release of the data to the community possible. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00018.SV and ADS/JAO.ALMA#2012.1.00453.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC 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. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). J.C. and A.F. thank the ERC for support under grant ERC-2013-Syg-610256-NANOCOSMOS. They also thank Spanish MINECO for funding support under grants AYA2012-32032, and from the CONSOLIDER Ingenio program “ASTROMOL” CSD 2009-00038. KS acknowledges grant 105-2119-M-001-036 from the Taiwanese Ministry of Science and Technology.
Paper: 2016MNRAS.463.3461S (acknowledgments)
We thank Lars Bildsten, Jared Brooks, Rob Farmer, Jason Ferguson, Ken Shen, and Frank Timmes for helpful discussions. We thank Marius Dan and Cody Raskin for providing the results of their SPH simulations as part of previous work. We thank Ken'ichi Nomoto, Todd Thompson, and Stan Woosley for useful conversations following the presentation of these results in preliminary form. We thank an anonymous referee for comments that led to improvements in the manuscript. We acknowledge stimulating workshops at Sky House and Palomar Observatory where these ideas germinated. JS is supported by the NSF Graduate Research Fellowship Program under grant DGE-1106400 and by NSF grant AST-1205732 . EQ is supported in part by a Simons Investigator award from the Simons Foundation and the David and Lucile Packard Foundation. This research is funded in part by the Gordon and Betty Moore Foundation through Grant GBMF5076 . DK was supported in part by a Department of Energy Office of Nuclear Physics Early Career Award, and by the Director, Office of Energy Research, Office of High Energy and Nuclear Physics, Divisions of Nuclear Physics, of the US Department of Energy under Contract no. DE-AC02-05CH11231 . This research used the SAVIO computational cluster resource provided by the Berkeley Research Computing program at the University of California Berkeley (supported by the UC Chancellor, the UC Berkeley Vice Chancellor of Research, and the Office of the CIO). This research has made use of NASA's Astrophysics Data System and GNU Parallel (Tange 2011 ).
Paper: 2015A&A...575A..48S (acknowledgments)
We thank Chris Pritchet and Dennis Zaritsky for help carrying out the MENeaCS spectroscopic survey, Patrick Kelly for making his python SLR code publicly available, and Radek Wojtak for suggesting an assessment of orientation bias. C.S., H.H., and M.V. acknowledge support from the European Research Council under FP7 grant number 279396. H.H., M.C. and R.F.J.vdB. acknowledge support from the Netherlands Organisation for Scientific Research grant number 639.042.814. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http:// [0]www. [0]sdss3. [0]org/. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of NASA’s Astrophysics Data System Bibliographic Services. This work has made use of the python packages scipy (http:// [0]www. [0]scipy. [0]org) and matplotlib (http:// [0]matplotlib. [0]org; Hunter 2007 ) and of IPython ( Pérez Granger 2007 ).
Paper: 2020ApJ...889..124T (acknowledgments)
We thank the referee for their careful reading of this paper and the very useful comments that greatly helped to improve the paper. P.T. and V.P. were funded for this work by the NASA Heliophysics Guest Investigator grant NNX15AF50G. P.T. was also supported by contracts 8100002705 and SP02H1701R from Lockheed Martin to SAO, and NASA contract NNM07AB07C to the Smithsonian Astrophysical Observatory. B.D.P. was supported by NASA contract NNG09FA40C ( IRIS ). This work has benefited from discussions at the International Space Science Institute (ISSI) meetings on “New Diagnostics of Particle Acceleration in Solar Coronal Nanoflares from Chromospheric Observations and Modeling,” and “Heating in the Magnetic Chromosphere,” where topics relevant to this work were discussed with other colleagues. 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. This research has made use of NASA’s Astrophysics Data System and of the SolarSoft package for IDL.
Paper: 2016ApJ...833..208M (acknowledgments)
The authors are especially grateful for the numerous discussions with Bidya Karak and Banibrata Mukhopadhyay. We thank the editor and the anonymous reviewer for comments that led to substantial improvements in the presentation of this paper. The authors are also thankful to Saikat Ghosh, Anand Jha, Aditya Kelkar, Anuj Nandi, Mahendra Verma, and Harshawardhan Wanare for helpful discussions. S.C. acknowledges financial support through the INSPIRE faculty award (DST/INSPIRE/04/2013/000365) conferred by the Indian National Science Academy (INSA) and the Department of Science and Technology (DST), India.
Paper: 2016ApJ...830...74A (acknowledgments)
We acknowledge AYA2014-54348-C3-1-R by MINECO/Spain and FEDER funds/EU (P.J.A., C.R.-L., and Z.M.B.); FPIBES-2011-049647 MINECO/Spain (Z.M.B.). A.R. acknowledges research funding from ERC Starting Grant 279347 and DFG Grant RE1664/9-2. M.Z. is funded through DFG Grant RE 1664/12-1. J.S.J. acknowledges funding by Fondecyt through grant 1161218 and partial supportfrom CATA-Basal (PB06, Conicyt).
Paper: 2018ApJ...869..180A (acknowledgments)
This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. 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 the National Aeronautics and Space Administration. This work made use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. V.M.K. is supported by a Lorne Trottier Chair in Astrophysics Cosmology, a Canada Research Chair, CIFAR, by an NSERC Discovery Grant and Herzberg Award, and by FRQNT/CRAQ. R.F.A. acknowledges support from an NSERC Postdoctoral Fellowship. P.S. is a Covington Fellow at DRAO. Facilities: Swift , NuSTAR , XMM-Newton . Software: astropy (Astropy Collaboration et al. 2013 ), xspec 12.8.2 ( http://xspec.gfsc.nasa.gov ), heasoft v6.19,6.20 ( https://heasarc.nasa.gov/lheasoft/ ), SAS v16.0 (Gabriel et al. 2004 ).
Paper: 2017ApJ...842...64T (acknowledgments)
F.T. thanks A. Bolatto and A. Marscher for useful comments. F.T. and C.S.R. acknowledges support for this work by the National Aeronautics and Space Administration (NASA) through Chandra Award Number GO4-15103A issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. F.T. acknowledges partial support by the Programma per Giovani Ricercatori-anno 2014 “Rita Levi Montalcini.” E.B. is supported by the European Unions Horizon 2020 research and innovation programme under the Marie Sklodowska Curie grant agreement No. 655324, and by the ICORE program of the Planning and Budgeting Committee (grant No. 1937/12).
Paper: 2017MNRAS.464.2120S (acknowledgments)
We thank François Lanusse, Anthony Pullen, Alex Geringer-Sameth, Sébastien Fromenteau and Shirley Ho for useful discussions related to this work. We also thank Uroš Seljak, Emmanuel Schaan, David Spergel and the anonymous referee for helpful feedback on this work. We thank Martin White and Beth Reid for providing us halo catalogue from simulations. We also thank the SDSS-I/II/III and Planck collaboration for their efforts in providing the data sets used in this work. RM acknowledges the support of the Department of Energy Early Career Award programme. SS acknowledges support from John Peoples Jr Presidential Fellowship from Carnegie Mellon University. Some of the results in this paper have been derived using the healpix package (Górski et al. 2005 ). 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/ . 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. Author Contributions . SS and RM contributed to the analysis and writing the paper. JB is an SDSS-III BOSS architect who contributed to the development of the BOSS survey.
Paper: 2016MNRAS.459.3395P (acknowledgments)
This work has been supported by the Agenzia Spaziale Italiana under the contract ASI-INAF 2015-039-R.O ‘Missione M4 di ESA: Partecipazione Italiana alla fase di assessment della missione THOR’. SP and GZ acknowledge support from the International Space Science Institute (ISSI) in Bern through the International Team no. 297 ‘Superdiffusive transport in space plasmas and its influence on energetic particle acceleration and propagation’.
Paper: 2018MNRAS.473.4698B (acknowledgments)
ACKNOWLEDGEMENTS We thank the anonymous referee for their constructive review, which helped improve the paper. We thank Rachel Mason for making the XDGNIRS reduction pipeline available. CMB acknowledges support from the Australian Government Research Training Program Scholarship. 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). RMcD is the recipient of an Australian Research Council Future Fellowship (project number FT150100333). CC acknowledges support from NASA grant NNX15AK14G, NSF grant AST-1313280 and the Packard Foundation.
Paper: 2017A&A...601A..97S (acknowledgments)
These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia -ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 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”. This work has been partially supported by PRIN-INAF-2014. The results presented here benefited from discussions held during the Gaia -ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. M.M. acknowledges financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F, from INAF through grant PRIN-2014-14, and from the MERAC Foundation. S.G.S. acknowledges the support by Fundação para a Ciência e Tecnologia (FCT) through national funds and a research grant (project Ref. UID/FIS/04434/2013, and PTDC/FIS-AST/7073/2014). S.G.S. also acknowledge the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program Programa Operacional de Factores de Competitividade COMPETE.
Paper: 2018A&A...617A.132D (acknowledgments)
Acknowledgements Based on observations made with APEX under programme IDs O-097.F-9318, O-098.F-9305, 077.F-9310, and 079.F-9325. This work is based on observations carried out under project number 010-13 with the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The Onsala 20 m telescope is operated by the Swedish National Facility for Radio Astronomy, Onsala Space Observatory at Chalmers University of Technology. L.D. acknowledges support from the ERC consolidator grant 646758 AEROSOL and the FWO Research Project grant G024112N. E.D.B. acknowledges financial support from the Swedish National Space Board. H.O. acknowledges financial support from the Swedish Research Council.
Paper: 2019ApJ...880...28Z (acknowledgments)
D.Z. and H.Z. acknowledge financial support from NSF grant AST-171384. J.W. acknowledges support from a 2018 Sloan Foundation Fellowship. The authors gratefully acknowledge the SDSS-III team for providing a valuable resource to the community. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website 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.
Paper: 2018MNRAS.475.2421S (acknowledgments)
ACKNOWLEDGEMENTS We would like to thank Eric Baxter, Joe DeRose, Ian Dell'Anotonio, Daniel Gruen, Hung-Jin Huang, Benjamin Joachimi, Andrey Kravtsov, Rachel Mandelbaum, Surhud More, Yuedong Fang, Mike Jarvis, Masahiro Takada, Joop Schaye, Frank van den Bosch, Mark Vogelsberger, Anja von der Linden, and Risa Wechsler for helpful discussions. We are very grateful to Erin Sheldon for allowing us to use his SDSS shear catalogues and source photometric redshift distributions. J.C., B.J., and G.B. are partially supported by the US Department of Energy grant DE-SC0007901 and funds from the University of Pennsylvania.
Paper: 2017MNRAS.470.2054C (acknowledgments)
Acknowledgments We are grateful to G. I. Ogilvie for his important remarks and suggestions. SVC and PBI were supported in part by RFBR grants 15-02-08476 and 16-02-01043, by programme 7 of the Presidium of Russian Academy of Sciences and also by Grant of the President of the Russian Federation for Support of the Leading Scientific Schools NSh-6595.2016.2.
Paper: 2017MNRAS.468.2532J (acknowledgments)
Acknowledgments We thank Elisa Costantini for helpful discussions and comments. CJ acknowledges valuable discussions with Lynne Valencic about the cosmic abundances. The anonymous referee is appreciated for providing insightful comments and suggestions, which allowed us to improve this paper significantly. We would also like to thank the XMMNewton team for providing important instructions on technical and calibration issues. This project is supported by the Bundesministerium fr Wirtschaft und Technologie/Deutsches Zentrum fr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408 and FKZ 50 OR 1604) and the Max Planck Society. This work is based on observations obtained with XMMNewton , an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. The scientific results reported in this paper are also based on observations made by the Chandra X-ray Observatory, as well as data obtained from the Chandra Data Archive. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages ciao , chips and sherpa .
Paper: 2018ApJ...862....8T (acknowledgments)
This paper makes use of the following ALMA data: ADS/ JAO.ALMA#2011.0.00611.S, 2012.1.00239.S, and 2015.1.00340.S. ALMA is a partnership of the ESO, NSF, NINS, NRC, NSC, and ASIAA. The Joint ALMA Observatory is operated by the ESO, AUI/NRAO, and NAOJ. This work was supported by NAOJ ALMA Scientific Research Grant Numbers 2016-03B and JSPS KAKENHI (Grant No. 22244014, 23403001, 26247026, 15K05039, and 18K13582).
Paper: 2016MNRAS.463..705C (acknowledgments)
We are grateful to the reviewer of this paper, Dr Bojan Novaković, for comments and suggestions that greatly improved the quality of this paper. We would like to thank the São Paulo State Science Foundation ( FAPESP ) that supported this work via the grant 2016/04476-8 , and the Brazilian National Research Council (CNPq, grant 305453/2011-4 ). This publication makes use of data products from the Wide-field Infrared Survey Explorer ( WISE ) and NEOWISE, which are 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: 2018ApJ...862..169A (acknowledgments)
We are grateful to the anonymous referee for constructive comments that significantly improved the manuscript. We are also grateful for the hospitality and financial support of the Max Planck Institute for Astrophysics that allowed IA to work directly with the MRS particle files in Garching, Germany. The Millennium Simulation databases used in this paper, and the web application providing online access to them, were constructed as part of the activities of the German Astrophysical Virtual Observatory. This work was partially supported by the National Science Foundation via grant AST-0708468.
Paper: 2018ApJ...852....4D (acknowledgments)
J.C.A.M.J. is the recipient of an Australian Research Council Future Fellowship (FT140101082). This work has been supported by the National Aeronautics and Space Administration through Chandra Award Number GO3-14046X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We are grateful for the contributions of Tom Maccarone, Mike Garcia, and Jerry Orosz, who provided crucial input in the initial design and execution of the observations. Facilities: CXO (ACIS) , VLA , CTIO:1.3 m. Software: CIAO (v4.8; Fruscione et al. 2006 ), CASA (v.4.2.0; McMullin et al. 2007 ), IRAF (v2.15.1a; Tody 1986 , 1993 ), Matplotlib (v2.0.2; Hunter 2007 ), Sherpa (Freeman et al. 2001 ).
Paper: 2015A&A...577A..60S (acknowledgments)
We are grateful to R. Trampedach for clarifications about his results, and for making available the routine to calculate Rosseland opacities. We also thank J. Christensen-Dalsgaard for interesting discussions on this topic, and the anonymous referee for comments that have improved the presentation of our results. S.C. gratefully acknowledges financial support from PRIN-INAF2014 (PI: S. Cassisi).
Paper: 2018A&A...609A..73R (acknowledgments)
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 the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. The author gratefully acknowledges support from the Spanish Ministry of Economy and Competitivity through project AYA2014-60476-P (Solar Magnetometry in the Era of Large Solar Telescopes). Part of this work was supported by the DFG grant RE 3282/1-2. This work has made use of the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna. We would like to thank the referee for the constructive suggestions.
Paper: 2019MNRAS.489.2634H (acknowledgments)
ACKNOWLEDGEMENTS We thank the anonymous referee for her/his suggested improvements. IB is supported by an Alexander von Humboldt postdoctoral research fellowship. KG was supported by the German-Russian Interdisciplinary Science Center funded by the German Federal Foreign Office via the German Academic Exchange Service. We thank Graeme Candlish for sharing his data on the velocity field in MOND cosmology and Hosein Haghi for useful discussions about the properties of NGC 1052-DF2.
Paper: 2016ApJ...826..141G (acknowledgments)
We thank the referee for the helpful comments that have helped us to improve the presentation of the paper. This work is supported by the National Basic Research Program (973 Program) of China (grants 2014CB845800) and the National Natural Science Foundation of China under grants 11543005, U1431124, and 11361140349 (China–Israel joint program).