Koss, Michael J. and Ricci, Claudio and Trakhtenbrot, Benny and Oh, Kyuseok and den Brok, Jakob S. and Mejía-Restrepo, Julian E. and Stern, Daniel and Privon, George C. and Treister, Ezequiel and Powell, Meredith C. and Mushotzky, Richard and Bauer, Franz E. and Ananna, Tonima T. and Baloković, Mislav and Bär, Rudolf E. and Becker, George and Bessiere, Patricia and Burtscher, Leonard and Caglar, Turgay and Congiu, Enrico and Evans, Phil and Harrison, Fiona and Heida, Marianne and Ichikawa, Kohei and Kamraj, Nikita and Lamperti, Isabella and Pacucci, Fabio and Ricci, Federica and Riffel, Rogério and Rojas, Alejandra F. and Schawinski, Kevin and Temple, Matthew J. and Urry, C. Megan and Veilleux, Sylvain and Williams, Jonathan (2022) BASS. XXII. The BASS DR2 AGN Catalog and Data. Astrophysical Journal Supplement Series, 261 (1). Art. No. 2. ISSN 0067-0049. doi:10.3847/1538-4365/ac6c05. https://resolver.caltech.edu/CaltechAUTHORS:20220726-997473000
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Abstract
We present the active galactic nucleus (AGN) catalog and optical spectroscopy for the second data release of the Swift BAT AGN Spectroscopic Survey (BASS DR2). With this DR2 release we provide 1449 optical spectra, of which 1182 are released for the first time, for the 858 hard-X-ray-selected AGNs in the Swift BAT 70-month sample. The majority of the spectra (801/1449, 55%) are newly obtained from Very Large Telescope (VLT)/X-shooter or Palomar/Doublespec. Many of the spectra have both higher resolution (R > 2500, N ∼ 450) and/or very wide wavelength coverage (3200–10000 Å, N ∼ 600) that are important for a variety of AGN and host galaxy studies. We include newly revised AGN counterparts for the full sample and review important issues for population studies, with 47 AGN redshifts determined for the first time and 790 black hole mass and accretion rate estimates. This release is spectroscopically complete for all AGNs (100%, 858/858), with 99.8% having redshift measurements (857/858) and 96% completion in black hole mass estimates of unbeamed AGNs (722/752). This AGN sample represents a unique census of the brightest hard-X-ray-selected AGNs in the sky, spanning many orders of magnitude in Eddington ratio (L/L_(Edd) = 10−5–100), black hole mass (M_(BH) = 10⁵–10¹⁰ M_⊙), and AGN bolometric luminosity (L_(bol) = 10⁴⁰–10⁴⁷ erg s⁻¹ ).
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| Additional Information: | © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 September 3; revised 2022 April 2; accepted 2022 April 10; published 2022 July 15. The BAT AGN Spectroscopic Survey Data Release 2. We thank the reviewer for the constructive comments that helped us improve the quality of this paper. BASS/DR2 was made possible through the coordinated efforts of a large team of astronomers, supported by various funding institutions, and using a variety of facilities. We acknowledge support from NASA through ADAP award NNH16CT03C (M.K.); the Israel Science Foundation through grant No. 1849/19 (B.T.); the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program, through grant agreement No. 950533 (B.T.); FONDECYT Postdoctorado 3180506 (F.R.) and 3210157 (A.R.); FONDECYT Regular 1190818 (E.T., F.E.B.) and 1200495 (E.T., F.E.B.); ANID grants CATA-Basal AFB-170002, ACE210002, and FB210003 (C.R., F.R., E.T., F.E.B., and E.C.); ANID Anillo ACT172033 (E.T.); Millennium Science Initiative Program—ICN12_009 (F.E.B.); an ESO fellowship (M.H., J.M.); and Fondecyt Iniciacion grant 11190831 (C.R.). K.O. acknowledges support from the National Research Foundation of Korea (NRF-2020R1C1C1005462) and the Japan Society for the Promotion of Science (JSPS, ID: 17321); I.L. acknowledges support from the Comunidad de Madrid through the Atracción de Talento Investigador Grant 2018-T1/TIC-11035, C.M.U. acknowledges support from the National Science Foundation under grant No. AST-1715512, F.P. acknowledges support from a Clay Fellowship administered by the Smithsonian Astrophysical Observatory, and from the Black Hole Initiative at Harvard University, which is funded by grants from the John Templeton Foundation and the Gordon and Betty Moore Foundation, M.B. acknowledges support from the YCAA Prize Postdoctoral Fellowship; R.R. thanks CNPq (311223/2020-6), CAPES, and FAPERGS (16/2551-0000251-7 and 19/2551-0001750-2). This work was performed in part at Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611. We also acknowledge the following people who assisted in acquiring the Palomar observations presented herein: Dave Alexander, Roberto Assef, Rosamaria Carraro, Alison Dugas, Peter Eisenhardt, Clarke Esmerian, Carla Fuentes, Felix Fuerst, Maya Fuller, Daniel Gawerc, David Girou, Ana Glidden, Matthew Graham, Claire Greenwell, Brian Grefenstette, Marianne Heida, Hyunsung Jun, Peter Kosec, Stephanie LaMassa, Jeff Maggio, Alejandra Melo, Catalina-Ana Miritescu, Wenli Mo, Eric Mukherjee, Gael Noirot, Antonija Oklopčić Sean Pike, Joseph Simon, Tawny Sit, Navin Sridhar, Aaron Stemo, Becky Tang, Thomas Venville, Jingyi Wang, and Dominika Wylezalek. We acknowledge financial contributions from Joanna Wall Muir and the California Institute of Technology's Student Faculty Program to assist in the Palomar observations for Tea Freedman-Susskind, Feiyang Liu, Milan Robertson, Yerong Xu, and Emily Zhang. We acknowledge the work that the Swift BAT team has done to make this project possible. We acknowledge the various telescopes used in this paper. We are tremendously thankful to all the observing and support staff in all the observatories, and their headquarters, for their great assistance in planning and conducting the observations that made BASS/DR2 possible. Specifically, BASS/DR2 is based on the following: (1) Observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under 34 ESO programs: 60.A-9024(A), 60.A-9421(A), 062.H-0612(A), 086.B-0135(A), 089.B-0951(A), 089.B-0951(B), 090.A-0830(A), 090.D-0828(A), 091.B-0900(B), 091.C-0934(B), 092.B-0083(A), 093.A-0766(A), 094.B-0321(A), 095.B-0059(A), 098.A-0062, 098.A-0635(B), 098.B-0551(A), 099.A-0403(A+B), 099.A-0442(A), 099.B-0785(A), 0101.A-0765(A), 0101.B-0456(B), 0101.B-0739(A), 0102.A-0433(A), 0102.B-0048, 0103.A-0521(A), 0103.B-0566(A), 0103.A-0777(A), 0104.A-0353(A), 0104.B-0959(A), 0106.A-0521(A), 385.B-1035(A), 2100.B-5018(B), and 60.A-9100(J). (2) Data obtained with the Hale 200-inch telescope at Palomar observatory, including five dedicated Yale programs: 2017B/Y04, 2018A/Y03, 2018B/Y04, 2019A/Y03, and 2019B/Y04 (PI: M. Powell). Additional data were obtained as part of Caltech runs including 2014B/P05, 2015A/P04, 2015B/P06, 2016A/P06, 2016B/P04, 2017A/P13, 2017B/P01, 2018A/P15, 2018B/P02, 2019A/P18, 2019B/P11, 2020A/P14, and 2020B/P19 (PI: F. Harrison) and also JPL runs including 2016B/J12, 2017A/J07, 2017B/J15 2019B/J09, 2019A/J06, 2019B/J19, 2020A/J11, and 2020B/J04 (PI: D. Stern). (3) Observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation's NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). These include from CNTAC (CN2018A-104, CN2018B-83) and NOIRLab program 2012A-0463 (PI M. Trippe). (4) Observations at Kitt Peak National Observatory at NSF's NOIRLab (NOIRLab Prop. ID 52, 2946; PI: F. Bauer), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. We 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. (5) Data gathered with the 6.5 m Magellan Telescopes (CN2019A-70 and CN2019B-77) and the 2.5 m du Pont telescope (CN2016A-80) located at Las Campanas Observatory, Chile. Support for the design and construction of the Magellan Echellette Spectrograph was received from the Observatories of the Carnegie Institution of Washington, the School of Science of the Massachusetts Institute of Technology, and the National Science Foundation in the form of a collaborative Major Research Instrument grant to Carnegie and MIT (AST0215989). (6) Data 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. (7) Data obtained as part of the various stages of the Sloan Digital Sky Survey (SDSS-I/II, III, and IV). Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the US Department of Energy Office of Science, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High Performance Computing at the University of Utah. The SDSS website is www.sdss.org. The most recent generation of the SDSS we benefited from, SDSS-IV, is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, Center for Astrophysics ∣ Harvard & Smithsonian, the Chilean Participation Group, the French Participation Group, Instituto de Astrofísica de Canarias, Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. 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 research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. A significant part of the BASS observations and work took place during the COVID-19 crisis. We thank the healthcare experts in communities around the world, for their tireless efforts to keep us all as safe and healthy as possible. Facilities: Du Pont (Boller & Chivens spectrograph), Keck:I (LRIS), Magellan:Clay, Hale (Doublespec), NuSTAR, Swift (XRT and BAT), VLT:Kueyen (X-shooter), VLT:Antu (FORS2), SOAR (Goodman). Software: Astropy (Collaboration et al. 2013), ESO Reflex (Freudling et al. 2013), IRAF (National Optical Astronomy Observatories 1999), Matplotlib (Hunter 2007), molecfit (Smette et al. 2015), Numpy (van der Walt et al. 2011), Pandas (https://doi.org/10.5281/zenodo.3630805), PySpecKit (Ginsburg & Mirocha 2011). | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Group: | Astronomy Department, Space Radiation Laboratory | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Subject Keywords: | X-ray active galactic nuclei; Active galactic nuclei; Seyfert galaxies; X-ray quasars; X-ray surveys; Surveys; Sky surveys; Galaxy spectroscopy | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Issue or Number: | 1 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Classification Code: | Unified Astronomy Thesaurus concepts: X-ray active galactic nuclei (2035); Active galactic nuclei (16); Seyfert galaxies (1447); X-ray quasars (1821); X-ray surveys (1824); Surveys (1671); Sky surveys (1464); Galaxy spectroscopy (2171) | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.3847/1538-4365/ac6c05 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20220726-997473000 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20220726-997473000 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Official Citation: | Michael J. Koss et al 2022 ApJS 261 2 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| ID Code: | 115856 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | George Porter | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 27 Jul 2022 21:23 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 27 Jul 2022 21:23 |
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