{
  "id": "1203.0239",
  "version": "v1",
  "published": "2012-03-01T16:33:48.000Z",
  "updated": "2012-03-01T16:33:48.000Z",
  "title": "A Combined Optical and X-ray Study of Unobscured Type 1 AGN. II. Relation Between X-ray Emission and Optical Spectra",
  "authors": [
    "C. Jin",
    "M. Ward",
    "C. Done"
  ],
  "comment": "23 pages, 14 figures, accepted by MNRAS",
  "categories": [
    "astro-ph.HE",
    "astro-ph.CO"
  ],
  "abstract": "In this paper we study the properties of the optical spectra of Type 1 active galactic nuclei (AGNs) by using the unobscured hard X-ray emission as a diagnostic. We develop the `Correlation Spectrum Technique' (CST) and use this to show the strength of correlation between the hard X-ray luminosity and each wavelength of the optical spectrum. This shows that for Broad Line Seyfert 1s all the strong emission lines (broad component of H\\alpha and H\\beta, [NeIII] \\lambda\\lambda 3869/3967, [OI] \\lambda\\lambda 6300/6364, [OII] \\lambda\\lambda 3726/3729, [OIII] \\lambda\\lambda 4959/5007) and the optical underlying continuum all strongly correlate with the hard X-ray emission. But the NLS1s appear to be somewhat different. Among the various Balmer line components and the broadband SED components, the best correlation exists between the hard X-ray component and broad component (BC) of the Balmer lines, which supports the view that broad line region (BLR) has the closest link with the AGN's compact X-ray emission. The equivalent widths of Balmer line IC and BC are found to correlate with L$_{2-10keV}$, $\\kappa_{2-10keV}^{-1} = L_{bol}/L_{2-10keV}$, Balmer line FWHM and black hole mass. There is a non-linear dependence of the Balmer line IC and BC luminosities with L$_{2-10keV}$ and L$_{5100}$, which suggests that a second-order factor such as the ILR and BLR covering factors affect the Balmer line component luminosities. The Balmer decrement is found to decrease from ~5 in the line core to ~2 in the extended wings, with mean decrements of 2.1 in BLR and 4.8 in ILR. This suggests different physical conditions in these regions. The [OIII] line is composed of a narrow core together with a blue-shifted component with average outflow velocity of $130^{+230}_{-80} km s^{-1}$. The total luminosity of [OIII] \\lambda 5007 well correlates with the hard X-ray luminosity.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2012-03-01T16:33:48.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "optical spectrum",
      "x-ray study",
      "unobscured type",
      "hard x-ray luminosity",
      "balmer line ic"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1111/j.1365-2966.2012.20847.x",
      "journal": "Monthly Notices of the Royal Astronomical Society",
      "year": 2012,
      "month": "Jun",
      "volume": 422,
      "number": 4,
      "pages": 3268
    },
    "note": {
      "typesetting": "TeX",
      "pages": 23,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1091255,
      "adsabs": "2012MNRAS.422.3268J"
    }
  }
}