{
  "id": "1406.6056",
  "version": "v2",
  "published": "2014-06-23T20:00:31.000Z",
  "updated": "2014-07-07T16:44:18.000Z",
  "title": "The distribution of satellites around massive galaxies at 1<z<3 in ZFOURGE/CANDELS: dependence on star formation activity",
  "authors": [
    "Lalitwadee Kawinwanichakij",
    "Casey Papovich",
    "Ryan F. Quadri",
    "Kim-Vy H. Tran",
    "Lee R. Spitler",
    "Glenn G. Kacprzak",
    "Ivo Labbe",
    "Caroline M. S. Straatman",
    "Karl Glazebrook",
    "Rebecca Allen",
    "Michael Cowley",
    "Romeel Davé",
    "Avishai Dekel",
    "Henry C. Ferguson",
    "W. G Hartley",
    "Anton M. Koekemoer",
    "David C. Koo",
    "Yu Lu",
    "Nicola Mehrtens",
    "Themiya Nanayakkara",
    "S. Eric Persson",
    "Glen Rees",
    "Brett Salmon",
    "Vithal Tilvi",
    "Adam R. Tomczak",
    "Pieter van Dokkum"
  ],
  "comment": "19 pages, 17 figures, accepted by ApJ. Information on ZFOURGE can be found at http://zfourge.tamu.edu",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "We study the statistical distribution of satellites around star-forming and quiescent central galaxies at 1<z<3 using imaging from the FourStar Galaxy Evolution Survey (ZFOURGE) and the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). The deep near-IR data select satellites down to $\\log(M/M_\\odot)>9$ at z<3. The radial satellite distribution around centrals is consistent with a projected NFW profile. Massive quiescent centrals, $\\log(M/M_\\odot)>10.78$, have $\\sim$2 times the number of satellites compared to star-forming centrals with a significance of 2.7$\\sigma$ even after accounting for differences in the centrals' stellar-mass distributions. We find no statistical difference in the satellite distributions of intermediate-mass quiescent and star-forming centrals, $10.48<\\log(M/M_\\odot)<10.78$. Comparing to the Guo2011 semi-analytic model, the excess number of satellites indicates that quiescent centrals have halo masses 0.3 dex larger than star-forming centrals, even when the stellar-mass distributions are fixed. We use a simple toy model that relates halo mass and quenching, which roughly reproduces the observed quenched fractions and the differences in halo mass between star-forming and quenched galaxies only if galaxies have a quenching probability that increases with halo mass from $\\sim$0 for $\\log(M_h/M_\\odot)\\sim$11 to $\\sim$1 for $\\log(M_h/M_\\odot)\\sim$13.5. A single halo-mass quenching threshold is unable to reproduce the quiescent fraction and satellite distribution of centrals. Therefore, while halo quenching may be an important mechanism, it is unlikely to be the only factor driving quenching. It remains unclear why a high fraction of centrals remain star-forming even in relatively massive halos.",
  "revisions": [
    {
      "version": "v2",
      "updated": "2014-07-07T16:44:18.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "star formation activity",
      "near-ir data select satellites",
      "deep extragalactic legacy survey",
      "near-ir deep extragalactic legacy",
      "massive galaxies"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1088/0004-637X/792/2/103",
      "journal": "The Astrophysical Journal",
      "year": 2014,
      "month": "Sep",
      "volume": 792,
      "number": 2,
      "pages": 103
    },
    "note": {
      "typesetting": "TeX",
      "pages": 19,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1302772,
      "adsabs": "2014ApJ...792..103K"
    }
  }
}