BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei

Creators: den Brok, Jakob S.; Koss, Michael J.; Trakhtenbrot, Benny; Stern, Daniel; Cantalupo, Sebastiano; Lamperti, Isabella; Ricci, Federica; Ricci, Claudio; Oh, Kyuseok; Bauer, Franz E.; Riffel, Rogerio; Rodríguez-Ardila, Alberto; Bär, Rudolf; Harrison, Fiona; Ichikawa, Kohei; Mejía-Restrepo, Julian E.; Mushotzky, Richard; Powell, Meredith C.; Boissay-Malaquin, Rozenn; Stalevski, Marko; Treister, Ezequiel; Urry, C. Megan; Veilleux, Sylvain

Abstract

We present the BAT AGN Spectroscopic Survey (BASS) Near-infrared Data Release 2 (DR2), a study of 168 nearby (z̅ = 0.04, z < 0.6) active galactic nuclei (AGN) from the all-sky Swift Burst Array Telescope X-ray survey observed with Very Large Telescope (VLT)/X-shooter in the near-infrared (NIR; 0.8 - 2.4 μm). We find that 49/109 (45%) Seyfert 2 and 35/58 (60%) Seyfert 1 galaxies observed with VLT/X-shooter show at least one NIR high-ionization coronal line (CL, ionization potential χ > 100 eV). Comparing the emission of the [Si vi] λ1.9640 CL with the X-ray emission for the DR2 AGN, we find a significantly tighter correlation, with a lower scatter (0.37 dex) than for the optical [O iii] λ5007 line (0.71 dex). We do not find any correlation between CL emission and the X-ray photon index Γ. We find a clear trend of line blueshifts with increasing ionization potential in several CLs, such as [Si vi] λ1.9640, [Si x] λ1.4300, [S viii] λ0.9915, and [S ix] λ1.2520, indicating the radial structure of the CL region. Finally, we find a strong underestimation bias in black hole mass measurements of Sy 1.9 using broad Hα due to the presence of significant dust obscuration. In contrast, the broad Paα and Paβ emission lines are in agreement with the M-σ relation. Based on the combined DR1 and DR2 X-shooter sample, the NIR BASS sample now comprises 266 AGN with rest-frame NIR spectroscopic observations, the largest set assembled to date.

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 2020 August 11; revised 2021 December 16; accepted 2021 December 28; published 2022 July 15. The BAT AGN Spectroscopic Survey Data Release 2. Based on observations collected under programs 086.B-0135(A), 089.B-0951(A), 090.A-0830(A), 091.B-0900(B), 093.A-0766(A), 098.A-0635(B), 099.A-0403(B), 0101.A-0765(A), and 0102.A-0433(A) with X-shooter at the Very Large Telescope of the Paranal Observatory in Chile, operated by the European Southern Observatory. We acknowledge support from NASA through ADAP award NNH16CT03C and 80NSSC19K0749 (M.J.K.); the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme through grant agreement No. 726384/Empire (J.S.d.B.); 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.); the Comunidad de Madrid through the Atracción de Talento Investigador Grant 2018-T1/TIC-11035 (I.L.); National Research Foundation of Korea award NRF-2020R1C1C1005462 (K.O.); the Japan Society for the Promotion of Science, ID: 17321 (K.O.); the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA (D.S.); Swiss National Science Foundation grants PP00P2_163824 and PP00P2_190092 (S.C.); the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme grant agreement No. 864361 (S.C.); ANID grants CATA-Basal AFB-170002 (F.E.B., F.R., E.T.) and ANID BASAL project FB210003 (F.E.B., C.R., E.T.), FONDECYT Regular 1190818 (E.T., F.E.B.) and 1200495 (F.E.B., E.T.), Fondecyt Iniciacion grant 11190831 (C.R.), FONDECYT Postdoctorado 3180506 (F.R.), and Millennium Science Initiative ICN12_009 (F.E.B.); Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), CAPES, and FAPERGS (R.R.); CNPq, through grant 312036/2019-1 (A.R.-A.); and the Ministry of Education, Science and Technological Development of the Republic of Serbia through contract No. 451-03-9/2021-14/200002 and the Science Fund of the Republic of Serbia, PROMIS 6060916, BOWIE (M.S.). This work was performed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611. Facilities: ESO-VLT - , Swift (BAT). - Software: astropy (Astropy Collaboration et al. 2013), Matplotlib (Hunter 2007), NumPy (van der Walt et al. 2011), Linmix (https://github.com/jmeyers314/linmix), PySpecKit v0.1.20 (Ginsburg & Mirocha 2011), ESO Reflex software v2.9.3 (Freudling et al. 2013), molecfit v1.5.9 (Kausch et al. 2015; Smette et al. 2015).

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