{
  "id": "2209.00014",
  "version": "v1",
  "published": "2022-08-31T18:00:00.000Z",
  "updated": "2022-08-31T18:00:00.000Z",
  "title": "BASS XXXVII: The role of radiative feedback in the growth and obscuration properties of nearby supermassive black holes",
  "authors": [
    "C. Ricci",
    "T. T. Ananna",
    "M. J. Temple",
    "C. M. Urry",
    "M. J. Koss",
    "B. Trakhtenbrot",
    "Y. Ueda",
    "D. Stern",
    "F. E. Bauer",
    "E. Treister",
    "G. C. Privon",
    "K. Oh",
    "S. Paltani",
    "M. Stalevski",
    "L. C. Ho",
    "A. C. Fabian",
    "R. Mushotzky",
    "C. S. Chang",
    "F. Ricci",
    "D. Kakkad",
    "L. Sartori",
    "R. Baer",
    "T. Caglar",
    "M. Powell",
    "F. Harrison"
  ],
  "comment": "Accepted for publication in ApJ",
  "categories": [
    "astro-ph.GA",
    "astro-ph.HE"
  ],
  "abstract": "We study the relation between obscuration and supermassive black hole (SMBH) growth using a large sample of hard X-ray selected Active Galactic Nuclei (AGN). We find a strong decrease in the fraction of obscured sources above the Eddington limit for dusty gas ($\\log \\lambda_{\\rm Edd}\\gtrsim -2$) confirming earlier results, and consistent with the radiation-regulated unification model. This also explains the difference in the Eddington ratio distribution functions (ERDFs) of type 1 and type 2 AGN obtained by a recent study. The break in the ERDF of nearby AGN is at $\\log \\lambda_{\\rm Edd}^{*}=-1.34\\pm0.07$. This corresponds to the $\\lambda_{\\rm Edd}$ where AGN transition from having most of their sky covered by obscuring material to being mostly devoid of absorbing material. A similar trend is observed for the luminosity function, which implies that most of the SMBH growth in the local Universe happens when the AGN is covered by a large reservoir of gas and dust. These results could be explained with a radiation-regulated growth model, in which AGN move in the $N_{\\rm H}-\\lambda_{\\rm Edd}$ plane during their life cycle. The growth episode starts with the AGN mostly unobscured and accreting at low $\\lambda_{\\rm Edd}$. As the SMBH is further fueled, $\\lambda_{\\rm Edd}$, $N_{\\rm H}$ and covering factor increase, leading AGN to be preferentially observed as obscured. Once $\\lambda_{\\rm Edd}$ reaches the Eddington limit for dusty gas, the covering factor and $N_{\\rm H}$ rapidly decrease, leading the AGN to be typically observed as unobscured. As the remaining fuel is depleted, the SMBH goes back into a quiescent phase.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-08-31T18:00:00.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "nearby supermassive black holes",
      "obscuration properties",
      "bass xxxvii",
      "radiative feedback",
      "x-ray selected active galactic"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}