adsabs/WIESP2022-NER huggingface dataset:
Paper: 2020ApJ...890...95I (acknowledgments)
This study makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00033.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 authors are grateful to Koichiro Nakanishi and Hiroshi Nagai for their valuable comments and useful website for ALMA data reduction. T.I. wishes to thank Mitaro Namiki of the Tokyo University of Agriculture and Technology and staff of the Information Technology Center of the University of Tokyo for their dedicated work and suggestions for the computing and understanding of the entire research works. The authors are grateful to an anonymous reviewer who gave important comments on manuscript from the professional point of view. This work was financially supported by a Telecommunications Advancement Foundation (T.I.), the Japan Society for the Promotion of Science (JSPS) Kakenhi grant (17K14420 and 19K14782, T.I.), and an Astrobiology Center Program of National Institutes of Natural Sciences (NINS) grant.
Paper: 2018MNRAS.477.2298Q (acknowledgments)
Acknowledgements LGQ is grateful to the Institute of Astronomy for hospitality during his stay. CAT thanks Churchill college for his fellowship. We thank the reviewer for helpful comments.
Paper: 2015ApJ...814...46H (acknowledgments)
We thank the anonymous referee for insightful comments which greatly improved the quality of this manuscript. This work is based on observations at the W.M. Keck Observatory, which is operated as a scientific partnership among Caltech, the University of California and NASA. S.H. wishes to thank B. Siana for very constructive comments and I. Shivaei for useful discussions. D.S. acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEst-OE/FIS/UI2751/2014.
Paper: 2016ApJ...818..149S (acknowledgments)
We dedicate this work to the memory of our dear colleague and co-author Dennis Lindle, who passed away during the writing of this paper. The authors thank J. Kaastra, T. R. Kallman, R. K. Smith, and E. M. Gullikson for stimulating conversations. W.C.S. and D.W.L. wish to acknowledge support by the National Science Foundation under NSF Grant No. PHY-09-70125. V.J. was funded by the European Social Fund under the Global Grant Measure (No. VP1-3.1-ŠMM-07-K-02-015). M.M.S. was supported by the CNPq-Brazil. D.W.S. was supported in part by the NASA Astrophysics Research and Analysis Program and the NASA Heliophysics Supporting Research Program. The experimental portion of this work was performed at the Advanced Light Source, which is supported by DOE (DE-AC03-76SF00098).
Paper: 2019A&A...632A..58R (acknowledgments)
Acknowledgements The authors thank the anonymous referee for their constructive comments that have improved the quality of the paper. The authors also thank Ana Duarte-Cabral, Paul Clark and Camilo Peñaloza for many helpful discussions relating to this work. A.J.R. would like to thank the STFC for postdoctoral support under the consolidated grant number ST/N000706/1, as well as funding for a Ph.D. studentship. S.E.R. acknowledges support from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement # 706 390. This research made use of Astropy ( https:// astropy.org/ ), a community-developed core Python package for Astronomy ( Astropy Collaboration 2013 , 2018 ), as well as iPython ( https://ipython.org/ ), an enhanced interactive Python ( Perez Granger 2007 ), and the Python packages NumPy ( https://numpy.org/ ; Oliphant 2006 ), SciPy ( https://scipy.org/ ; Jones et al. 2001 ), and Matplotlib ( https://matplotlib.org/ ; Hunter 2007 ). This publication has also made use of TOPCAT ( http://www.star.bris.ac.uk/~mbt/topcat/ ), an interactive graphical viewer and editor for tabular data software ( Taylor 2005 ), and SAOImageDS9 ( http://ds9.si.edu/ ; Joye Mandel 2003 ), an astronomical imaging and data-visualization application. 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. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency, and has made use of the NASA Astrophysical Data System. The Starlink software ( Currie et al. 2014 ) is currently supported by the East Asian Observatory.
Paper: 2019ApJ...886...66N (acknowledgments)
We thank the anonymous referee, whose comments improved the clarity of the manuscript. M.N. acknowledges the support from the Vacation Scholarship program at the Centre for Astrophysics Supercomputing at Swinburne University of Technology. N.M.N. and G.G.K. acknowledge the support of the Australian Research Council through a Discovery Project DP170103470. S.K.P. acknowledges support through the Australian Government Research Training Program Scholarship. Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project No. CE170100012. S.M. acknowledges support from European Research Council (ERC), Grant Agreement 278594-GasAroundGalaxies. C.W.C. and J.C.C. acknowledge the support from award 1517831 from the National Science Foundation. J.C.C. is also supported by National Science Foundation grant AST-1312686. This work made use of Python packages NumPy and SciPy (Oliphant 2007 ), Matplotlib (Hunter 2007 ), IPython (Pérez Granger 2007 ), tqdm (da Costa-Luis et al. 2018 ), and Numba (Lam et al. 2015 ) and of NASA’s Astrophysics Data System Bibliographic Services. Galaxy data presented here 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. Observations were supported by Swinburne Keck programs 2014A_W178E, 2014B_W018E, 2015_W018E, and 2016A_W056E. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Facility: Keck:II (ESI).
Paper: 2018MNRAS.474.2564K (acknowledgments)
Acknowledgements We are grateful to Mark Booth for commenting on the manuscript and Hiroshi Kobayashi for providing us with the details of his planetesimal growth simulations. A speedy and insightful referee report by an anonymous reviewer is very much appreciated. AVK, TL, and JB thank the Deutsche Forschungsgemeinschaft (DFG) for financial support through grants Kr 2164/13-1, Lo 1715/2-1, and Bl 298/24-1, respectively. AJ thanks the Knut and Alice Wallenberg Foundation (grants 2012.0150, 2014.0017, 2014.0048), the Swedish Research Council (grant 2014-5775) and the European Research Council (ERC Consolidator Grant 724687-PLANETESYS) for their financial support.
Paper: 2018MNRAS.473.2434W (acknowledgments)
Acknowledgements I would like to thank Charalampos Markakis, Volker Perlick and Pavel Jefremov for useful discussions on this topic. I am also grateful for the support from a PhD grant of the German Research Foundation within its Research Training Group 1620 Models of Gravity .
Paper: 2017MNRAS.470.4662P (acknowledgments)
Acknowledgements We thank the anonymous referee for very helpful comments and suggestions. The ASTE project is led by Nobeyama Radio Observatory (NRO), a branch of National Astronomical Observatory of Japan (NAOJ), in collaboration with University of Chile and Japanese institutes including University of Tokyo, Nagoya University, Osaka Prefecture University, Ibaraki University, Hokkaido University and the Joetsu University of Education. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. SP, MO and AP are members of the Carrera del investigador científico of CONICET, Argentina. MCP is a doctoral fellow of CONICET, Argentina. This work was partially supported by grants awarded by CONICET, ANPCYT and UBA (UBACyT) from Argentina. AP acknowledges support from the Varsavsky Foundation. MR acknowledges support from FONDECYT(CHILE) grant No. 1140839. SP and AP are grateful to Dr Takeshi Okuda for the support received during the ASTE observations.
Paper: 2017MNRAS.467.1008P (acknowledgments)
Acknowledgments EP acknowledges the Jeremiah Horrocks Institute of the University of Central Lancashire for the hospitality while this paper was in progress. EP was partially supported by Accademia Nazionale dei Lincei and Fondazione Ing. Aldo Gini. Additional support while the paper was completed was provided by the Italian Ministry for Education University and Research (MIUR). VPD was supported by STFC Consolidated grants no. ST/J001341/1 and no. ST/M000877/1. VPD acknowledges being a part of the network supported by the COST Action TD1403 Big Data Era in Sky and Earth Observation. DRC was supported by STFC Consolidated grant no. ST/J001341/1. EMC, EDB, LM and AP are supported by Padua University through grants 60A02-5857/13, 60A02-5833/14 and 60A02-4434/15 and BIRD 164402/16. The simulation was run at the DiRAC Shared Memory Processing system at the University of Cambridge, operated by the COSMOS Project at the Department of Applied Mathematics and Theoretical Physics on behalf of the STFC DiRAC HPC Facility ( www.dirac.ac.uk ). This equipment was funded by BIS National E-infrastructure capital grant ST/J005673/1, STFC capital grant ST/H008586/1 and STFC DiRAC Operations grant ST/K00333X/1. DiRAC is part of the National E-Infrastructure. EP would like to thank R. Ragazzoni for his support while this work was in progress.
Paper: 2015ApJ...814..105H (acknowledgments)
This work was supported by NASA through grants NNX14AG05G, NNX14AC05G, and NNX09AB04G. We thank the SDO team for the use of AIA/SDO data. R.J. would like to acknowledge the support of the University of Sheffield (UK) and thanks R. Maurya for discussions regarding AIA/SDO images.
Paper: 2019A&A...632A..39V (acknowledgments)
We acknowledge the financial support by the Academy of Finland to the ReSoLVE Centre of Excellence (project no. 307411). The National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy, AURA Inc under cooperative agreement with the National Science Foundation (NSF). The data used in this work were produced in the framework of the NSO synoptic program. HMI data are courtesy of the Joint Science Operations Center (JSOC) Science Data Processing team at Stanford University. This work was partially supported by the International Space Science Institute (Bern, Switzerland) via International Team 420 on Reconstructing Solar and Heliospheric Magnetic Field Evolution over the Past Century.
Paper: 2019A&A...622A.150J (acknowledgments)
This research has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 682462) and is supported by the Research Council of Norway through its Centres of Excellence scheme, project number 262622. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00020.SV. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), 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. 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 AIA and HMI data are courtesy of the NASA/SDO, as well as AIA and HMI science teams. SJ is grateful to L. Rouppe van der Voort, S.K. Solanki, T.M.D. Pereira, and L. Mas-Ribas for useful discussions.
Paper: 2016ApJ...831..208H (acknowledgments)
Construction of the LWA has been supported by the Office of Naval Research under Contract N00014-07-C-0147. Support for operations and continuing development of LWA-1 is provided by the National Science Foundation under Grant AST-1139974 of the University Radio Observatory program. Thanks are due to NASA and NRL for their maintenance and provision of the SOHO and SDO data sets and to C. de Koning for producing the base-difference images in Figure 1 . T.A.H. is supported in part by the NSF SHINE Competition (Grant AGS-1260321), the NASA H-GI program (Grant NNX13AE01G), and the AFOSR program (Grant FA9550-14-0296).
Paper: 2018MNRAS.480...17M (acknowledgments)
ACKNOWLEDGEMENTS We are grateful to Dr. R. Matsumoto, Dr. K. Takahashi, and Dr. S. Ideguchi for useful discussion. We thank to Mr. Y. Morita who helped us a part of the visualization. We also thank to anomalous referee whose comments are very useful to improve our manuscript. Numerical computations were carried out on SX-9 and XC30 at the Center for Computational Astrophysics, CfCA of NAOJ (P.I. MM). A part of this research used computational resources of the HPCI system provided by (FX10 of Kyushu University) through the HPCI System Research Project (Project ID:hp140170).This work is financially supported in part by a Grant-in-Aid for Scientific Research (KAKENHI) from JSPS (P.I. MM:23740153, 16H03954, TA:15K17614, 15H03639).
Paper: 2019ApJ...874....4A (acknowledgments)
We thank J. Bernal, L. Verde, and D. Scolnic for useful conversations and E. Calabrese for providing the ACTpol r s constraint in Figure 3 . We use the CosmoSlik package Millea ( 2017 ) to sample our results. The work of K.A. and L.K. was supported in part by NSF support for the South Pole Telescope collaboration via grant OPP-1248097. The work of M.J. was supported via the NSF REU program at UC Davis via grant PHY-1560482. S.R. is supported by the Australian Research Council’s Discovery Projects scheme via grant DP150103208. W.L.K.W. was supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through an endowment from the Kavli Foundation and its founder, Fred Kavli.
Paper: 2016MNRAS.455.4122B (acknowledgments)
We are grateful to A. Montero-Dorta for helpful discussions about his work, and the staff of the LYTE centre for its hospitality when this work was completed.
Paper: 2019ApJ...877...34H (acknowledgments)
We thank the anonymous referee for detailed comments. This work is supported by the Ministry of Science and Technology, Taiwan, through grants MOST 105-2119-M-007-029-MY3 and 106-2112-M-007-006-MY3. Software: IPython (Pérez Granger 2007 ), Matplotlib (Hunter 2007 ), NumPy (van der Walt et al. 2011 ), SciPy (Jones et al. 2001 ), SymPy (Meurer et al. 2017 ).
Paper: 2019A&A...624A..46L (acknowledgments)
Acknowledgements We thank the anonymous referee for his useful comments and suggestions. The authors acknowledge support from the Swiss NCCR PlanetS and the Swiss National Science Foundation. We thank Juan Cabrera for useful discussions. J.S. is grateful to Françoise Roques for preliminary discussions. P. R. acknowledges financial support from the Programme National de Planétologie (INSU-CNRS). A.C. acknowledges support from projects UID/FIS/04564/2019, POCI-01-0145-FEDER-022217, and POCI-01-0145-FEDER-029932, funded by COMPETE 2020 and FCT, Portugal. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche.
Paper: 2017ApJ...835..219A (acknowledgments)
The Fermi -LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. W.L. was supported by NASA HGI grant NNX16AF78G and LWS grant NNX14AJ49G. V.P., W.L., and F.R.d.C. are supported by NASA grants NNX14AG03G, NNX13AF79G, and NNX12AO70G. V.P. and L.K. are grateful for RFBR grant 15-02-03717. We thank Nariaka Nitta and Meng Jin for friutful discussions on SEPs and magnetic connectivity.
Paper: 2019ApJ...878...61N (acknowledgments)
We are grateful to the anonymous referee for offering constructive comments, which have contributed to substantially improving this paper. The VLBA and the VLA are operated by the National Radio Astronomy Observatory. 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 (NASA). The study was partially supported by the Sasakawa Scientific Research Grant of The Japan Science Society (SN, 28-220) and by Grants-in-Aid for Scientific Research (B) (24340042, AD) of the Japan Society for the Promotion of Science (JSPS).
Paper: 2019A&A...623A...2A (acknowledgments)
NC kindly acknowledges support by the AvH foundation and MPIK, and FMR by a DFG Heisenberg Fellowship (RI 1187/4-1). We thank Werner Hofmann and Luigi Tibaldo for insightful comments. We also thank the referee for the comments that were useful in improving the paper.
Paper: 2017ApJ...835...35H (acknowledgments)
We thank the referee for valuable suggestions and comments that greatly improved the paper. The data used here are courtesy of the NVST, SDO , WIND , RHESSI , and GOES science teams. NVST is jointly operated and administrated by Yunnan Observatories and Center for Astronomical Mega-Science, Chinese Academy of Science. This work is supported by the Natural Science Foundation of China under grants 11333007, 11403098, 11573012, 11503081, 11503082, and 11633008, and the CAS “Light of West China” Program.
Paper: 2019ApJ...877...37R (acknowledgments)
M.R.M. and A.M.G. are supported by NSF grants AST-0909218 and AST-1412615. A.M.G. is also supported by the Lauren Leichtman Arthur Levine Chair in Astrophysics. This work is based on observations made with the NASA/ESA Hubble Space Telescope , obtained the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 11671, 12667, 12318, and 14613. We thank the anonymous referee for their thorough reading and insightful comments, which improved the content and presentation of this paper. Facility: HST (WFC3-IR). Software: Astropy (The Astropy Collaboration et al. 2013 ), IPython (Pérez Granger 2007 ), Matplotlib (Hunter 2007 ), NumPy (Oliphant 2007 ; van der Walt et al. 2011 ), SciPy (Jones et al. 2001 ; Oliphant 2007 ; Millman Aivazis 2011 ), MultiNest (Feroz et al. 2009 ), PyMultiNest (Buchner et al. 2014 ).
Paper: 2016A&A...595A.126M (acknowledgments)
We thank the anonymous referee for useful comments which helped to improve the paper. 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. The authors thank its members, as well as Liyi Gu and Craig Sarazin for helpful discussions. P.K. thanks Steve Allen and Ondrej Urban for support and hospitality at Stanford University. Y.Y.Z. acknowledges support from the German BMWI through the Verbundforschung under grant 50 OR 1506. 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 Space Research.
Paper: 2015ApJ...808...38R (acknowledgments)
The authors wish to thank Sara Ellison, Crystal Martin, and George Djorgovski for aiding in collection and reduction of the Keck/ESI spectroscopy used in this study. We also wish to thank the anonymous referee for useful comments which improved the manuscript. It is our pleasure to thank Neil Crighton, Simeon Bird, Jeff Cooke, Claude-André Faucher-Giguère, Michele Fumagalli, John O’Meara, Celine Péroux, Ali Rahmati, and Sijing Shen for valuable discussion of this work, and to acknowledge Sijing Shen for sharing the results of her analysis of the CGM properties of the Eris2 simulation. Finally, we are grateful to Art Wolfe for sharing his insight on these results and for his inspiring and pioneering work in this field. K.H.R.R. acknowledges the generous support of the Clay Postdoctoral Fellowship, and J.F.H. acknowledges support from the Alexander von Humboldt foundation in the context of the Sofja Kovalevskaja Award. The Humboldt foundation is funded by the German Federal Ministry for Education and Research. J.X.P. and M.L. acknowledge support from National Science Foundation (NSF) grants AST-1010004, AST-1109452, AST-1109447, and AST-1412981. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Some 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: 2019ApJ...875...29M (acknowledgments)
We thank the referee for giving suggestions that improved the paper. We warmly thank the California- Kepler Survey team for making their reduced data publicly available. We thank the European Space Agency (ESA) mission Gaia and NASA Exoplanet Archive for the data used in this work. C.M. acknowledges the financial support from Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq). C.M. also thanks D.F. Morell for his kindly assistance in the R language. K.C. and V.S. acknowledge that their work is supported in part by the National Aeronautics and Space Administration under grant 16-XRP16 2-0004, issued through the Astrophysics Division of the Science Mission Directorate. L.G. is thankful for the financial support from Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES). Software: Python packages: astropy (Astropy Collaboration et al. 2013 ), isoclassify (Huber et al. 2017 ); and R packages: astro (Lee 2014 ), mclust (Scrucca et al. 2016 ), MASS (Venables Ripley 2002 ).