{
  "id": "1404.6795",
  "version": "v2",
  "published": "2014-04-27T17:26:25.000Z",
  "updated": "2014-05-03T16:59:16.000Z",
  "title": "Evidence for AGN Feedback in the Broad Absorption Lines and Reddening of Mrk 231",
  "authors": [
    "Karen M. Leighly",
    "Donald M. Terndrup",
    "Eddie Baron",
    "Adrian B. Lucy",
    "Matthias Dietrich",
    "Sarah C. Gallagher"
  ],
  "comment": "Accepted for publication in the Astrophysical Journal, replaced Figure 6",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We present the first J-band spectrum of Mrk 231, which reveals a large \\ion{He}{1}*$\\lambda 10830$ broad absorption line with a profile similar to that of the well-known \\ion{Na}{1} broad absorption line. Combining this spectrum with optical and UV spectra from the literature, we show that the unusual reddening noted by \\citet{veilleux13} is explained by a reddening curve like those previously used to explain low values of total-to-selective extinction in SNe Ia. The nuclear starburst may be the origin and location of the dust. Spatially-resolved emission in the broad absorption line trough suggests nearly full coverage of the continuum emission region. The broad absorption lines reveal higher velocities in the \\ion{He}{1}* lines (produced in the quasar-photoionized \\ion{H}{2} region) compared with the \\ion{Na}{1} and \\ion{Ca}{2} lines (produced in the corresponding partially-ionized zone). {\\it Cloudy} simulations show that a density increase is required between the \\ion{H}{2} and partially-ionized zones to produce ionic column densities consistent with the optical and IR absorption line measurements and limits, and that the absorber lies $\\sim 100\\rm \\, pc$ from the central engine. These results suggest that the \\ion{He}{1}* lines are produced in an ordinary quasar BAL wind that impacts upon, compresses, and accelerates the nuclear starburst's dusty effluent (feedback in action), and the \\ion{Ca}{2} and \\ion{Na}{1} lines are produced in this dusty accelerated gas. This unusual circumstance explains the rarity of \\ion{Na}{1} absorption lines; without the compression along our line of sight, Mrk~231 would appear as an ordinary FeLoBAL.",
  "revisions": [
    {
      "version": "v2",
      "updated": "2014-05-03T16:59:16.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "agn feedback",
      "broad absorption lines reveal higher",
      "produce ionic column densities consistent",
      "absorption lines reveal higher velocities"
    ],
    "publication": {
      "doi": "10.1088/0004-637X/788/2/123",
      "journal": "The Astrophysical Journal",
      "year": 2014,
      "month": "Jun",
      "volume": 788,
      "number": 2,
      "pages": 123
    },
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "adsabs": "2014ApJ...788..123L"
    }
  }
}