{
  "id": "1504.05209",
  "version": "v1",
  "published": "2015-04-20T20:09:31.000Z",
  "updated": "2015-04-20T20:09:31.000Z",
  "title": "Stellar and Quasar Feedback in Concert: Effects on AGN Accretion, Obscuration, and Outflows",
  "authors": [
    "Philip F. Hopkins",
    "Paul Torrey",
    "Claude-Andre Faucher-Giguere",
    "Eliot Quataert",
    "Norman Murray"
  ],
  "comment": "13 pages, 9 figures. Submitted to MNRAS. Comments welcome",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO",
    "astro-ph.HE"
  ],
  "abstract": "We use hydrodynamic simulations to study the interaction of realistic active galactic nucleus (AGN) feedback mechanisms (accretion-disk winds & Compton heating) with a multi-phase interstellar medium (ISM). Our ISM model includes radiative cooling and explicit stellar feedback from multiple processes. We simulate radii ~0.1-100 pc around an isolated (non-merging) black hole. These are the scales where the accretion rate onto the black hole is determined and where AGN-powered winds and radiation couple to the ISM. Our primary results include: (1) The black hole accretion rate on these scales is determined by exchange of angular momentum between gas and stars in gravitational instabilities. This produces accretion rates of ~0.03-1 Msun/yr, sufficient to power a luminous AGN. (2) The gas disk in the galactic nucleus undergoes an initial burst of star formation followed by several Myrs where stellar feedback suppresses the star formation rate per dynamical time. (3) AGN winds injected at small radii with momentum fluxes ~L/c couple efficiently to the ISM and have a dramatic effect on the ISM properties in the central ~100 pc. AGN winds suppress the nuclear star formation rate by a factor of ~10-30 and the black hole accretion rate by a factor of ~3-30. They increase the total outflow rate from the galactic nucleus by a factor of ~10. The latter is broadly consistent with observational evidence for galaxy-scale atomic and molecular outflows driven by AGN rather than star formation. (4) In simulations that include AGN feedback, the predicted column density distribution towards the black hole is reasonably consistent with observations, whereas absent AGN feedback, the black hole is isotropically obscured and there are not enough optically-thin sight lines to explain observed Type I AGN. A 'torus-like' geometry arises self-consistently because AGN feedback evacuates the gas in the polar regions.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2015-04-20T20:09:31.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "black hole accretion rate",
      "agn accretion",
      "quasar feedback",
      "galactic nucleus",
      "star formation rate"
    ],
    "publication": {
      "doi": "10.1093/mnras/stw289"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 13,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1362455
    }
  }
}