TY - JOUR
T1 - BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
AU - Ananna, Tonima Tasnim
AU - Weigel, Anna K.
AU - Trakhtenbrot, Benny
AU - Koss, Michael J.
AU - Urry, C. Megan
AU - Ricci, Claudio
AU - Hickox, Ryan C.
AU - Treister, Ezequiel
AU - Bauer, Franz E.
AU - Ueda, Yoshihiro
AU - Mushotzky, Richard
AU - Ricci, Federica
AU - Oh, Kyuseok
AU - Mejía-Restrepo, Julian E.
AU - Brok, Jakob Den
AU - Stern, Daniel
AU - Powell, Meredith C.
AU - Caglar, Turgay
AU - Ichikawa, Kohei
AU - Wong, O. Ivy
AU - Harrison, Fiona A.
AU - Schawinski, Kevin
N1 - Funding Information:
We thank the anonymous reviewers for their constructive and detailed comments, which helped us improve the quality of this paper. T.T.A. and R.C.H. acknowledge support from NASA, through ADAP award 80NSSC19K0580. R.C.H. also acknowledges support from the National Science Foundation, through CAREER award 1554584. B.T. acknowledges support from the Israel Science Foundation (grant No. 1849/19) and from the European Research Council (ERC), under the European Union’s Horizon 2020 research and innovation program (grant agreement number 950533). M.K. acknowledges support from NASA, through ADAP award NNH16CT03C. C.M.U. acknowledges support from the National Science Foundation, under grant No. AST-1715512. C.R. acknowledges support from the Fondecyt Iniciacion, grant 11190831. We acknowledge support from ANID-Chile Basal AFB-170002 and FB210003 (E.T., F.E.B.), FONDECYT Regular 1200495 and 1190818 (E.T., F.E.B.), ANID Anillo ACT172033 (E.T.), Millennium Nucleus NCN19_058 (TITANs; E.T.), and the Millennium Science Initiative Program—ICN12_009 (F.E.B.). K.O. acknowledges support from the National Research Foundation of Korea (NRF-2020R1C1C1005462). The work of K.I. is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI (18K13584, 20H01939). J.d.B. acknowledges funding from the European Research Council (ERC), under the European Union’s Horizon 2020 research and innovation program (grant agreement No.726384/Empire). This work was performed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/7/1
Y1 - 2022/7/1
N2 - We determine the low-redshift X-ray luminosity function, active black hole mass function (BHMF), and Eddington ratio distribution function (ERDF) for both unobscured (Type 1) and obscured (Type 2) active galactic nuclei (AGNs), using the unprecedented spectroscopic completeness of the BAT AGN Spectroscopic Survey (BASS) data release 2. In addition to a straightforward 1/V max approach, we also compute the intrinsic distributions, accounting for sample truncation by employing a forward-modeling approach to recover the observed BHMF and ERDF. As previous BHMFs and ERDFs have been robustly determined only for samples of bright, broad-line (Type 1) AGNs and/or quasars, ours are the first directly observationally constrained BHMF and ERDF of Type 2 AGNs. We find that after accounting for all observational biases, the intrinsic ERDF of Type 2 AGNs is significantly more skewed toward lower Eddington ratios than the intrinsic ERDF of Type 1 AGNs. This result supports the radiation-regulated unification scenario, in which radiation pressure dictates the geometry of the dusty obscuring structure around an AGN. Calculating the ERDFs in two separate mass bins, we verify that the derived shape is consistent, validating the assumption that the ERDF (shape) is mass-independent. We report the local AGN duty cycle as a function of mass and Eddington ratio, by comparing the BASS active BHMF with the local mass function for all supermassive black holes. We also present the logN-logS of the Swift/BAT 70 month sources.
AB - We determine the low-redshift X-ray luminosity function, active black hole mass function (BHMF), and Eddington ratio distribution function (ERDF) for both unobscured (Type 1) and obscured (Type 2) active galactic nuclei (AGNs), using the unprecedented spectroscopic completeness of the BAT AGN Spectroscopic Survey (BASS) data release 2. In addition to a straightforward 1/V max approach, we also compute the intrinsic distributions, accounting for sample truncation by employing a forward-modeling approach to recover the observed BHMF and ERDF. As previous BHMFs and ERDFs have been robustly determined only for samples of bright, broad-line (Type 1) AGNs and/or quasars, ours are the first directly observationally constrained BHMF and ERDF of Type 2 AGNs. We find that after accounting for all observational biases, the intrinsic ERDF of Type 2 AGNs is significantly more skewed toward lower Eddington ratios than the intrinsic ERDF of Type 1 AGNs. This result supports the radiation-regulated unification scenario, in which radiation pressure dictates the geometry of the dusty obscuring structure around an AGN. Calculating the ERDFs in two separate mass bins, we verify that the derived shape is consistent, validating the assumption that the ERDF (shape) is mass-independent. We report the local AGN duty cycle as a function of mass and Eddington ratio, by comparing the BASS active BHMF with the local mass function for all supermassive black holes. We also present the logN-logS of the Swift/BAT 70 month sources.
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U2 - 10.3847/1538-4365/ac5b64
DO - 10.3847/1538-4365/ac5b64
M3 - Article
AN - SCOPUS:85133522841
SN - 0067-0049
VL - 261
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 1
M1 - 9
ER -