{
  "id": "2006.10128",
  "version": "v1",
  "published": "2020-06-17T19:58:44.000Z",
  "updated": "2020-06-17T19:58:44.000Z",
  "title": "The (black hole mass)-(color) relations for early- and late-type galaxies: red and blue sequences",
  "authors": [
    "Bililign T. Dullo",
    "Alexandre Y. K. Bouquin",
    "Armando Gil De Paz",
    "Johan H. Knapen",
    "Javier Gorgas"
  ],
  "comment": "27 pages, 8 figures, 6 tables, accepted for publication in ApJ",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "[Abridged] Tight correlations between supermassive black hole (SMBH) mass ($M_{\\rm BH}$) and the properties of the host galaxy have useful implications for our understanding of the growth of SMBHs and evolution of galaxies. Here, we present newly observed correlations between $M_{\\rm BH}$ and the host galaxy total UV$-$ [3.6] color ($\\mathcal{C_{\\rm UV,tot}}$, Pearson's r = $0.6-0.7$) for a sample of 67 galaxies (20 early-type galaxies and 47 late-type galaxies) with directly measured $M_{\\rm BH}$ in the GALEX/S$^{4}$G survey. The colors are carefully measured in a homogeneous manner using the galaxies' FUV, NUV and 3.6 $\\micron$ magnitudes and their multi-component structural decompositions in the literature. We find that more massive SMBHs are hosted by (early- and late-type) galaxies with redder colors, but the $M_{\\rm BH}- \\mathcal{C_{\\rm UV,tot}}$ relations for the two morphological types have slopes that differ at $\\sim 2 \\sigma$ level. Early-type galaxies define a red sequence in the $M_{\\rm BH}- \\mathcal{C_{\\rm UV,tot}}$ diagrams, while late-type galaxies trace a blue sequence. Within the assumption that the specific star formation rate of a galaxy (sSFR) is well traced by $L_{\\rm UV}/L_{\\rm 3.6}$, it follows that the SMBH masses for late-type galaxies exhibit a steeper dependence on sSFR than those for early-type galaxies. The $M_{\\rm BH}- \\mathcal{C_{\\rm UV,tot}}$ and $M_{\\rm BH}-L_{\\rm 3.6,tot}$ relations for the sample galaxies reveal a comparable level of vertical scatter in the log $M_{\\rm BH}$ direction, roughly $5\\%-27\\%$ more than the vertical scatter of the $M_{\\rm BH}-\\sigma$ relation. Our $M_{\\rm BH}- \\mathcal{C_{\\rm UV,tot}}$ relations suggest different channels of SMBH growth for early- and late-type galaxies, consistent with their distinct formation and evolution scenarios.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2020-06-17T19:58:44.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "black hole mass",
      "blue sequence",
      "host galaxy total uv",
      "specific star formation rate",
      "early-type galaxies define"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 27,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}