{
  "id": "1612.01088",
  "version": "v1",
  "published": "2016-12-04T09:10:07.000Z",
  "updated": "2016-12-04T09:10:07.000Z",
  "title": "Clustering of infrared-bright dust-obscured galaxies revealed by the Hyper Suprime-Cam and WISE",
  "authors": [
    "Yoshiki Toba",
    "Tohru Nagao",
    "Masaru Kajisawa",
    "Taira Oogi",
    "Masayuki Akiyama",
    "Hiroyuki Ikeda",
    "Jean Coupon",
    "Michael A. Strauss",
    "Wei-Hao Wang",
    "Masayuki Tanaka",
    "Mana Niida",
    "Masatoshi Imanishi",
    "Chien-Hsiu Lee",
    "Hideo Matsuhara",
    "Yoshiki Matsuoka",
    "Masafusa Onoue",
    "Yuichi Terashima",
    "Yoshihiro Ueda",
    "Yuichi Harikane",
    "Yutaka Komiyama",
    "Satoshi Miyazaki",
    "Akatoki Noboriguchi",
    "Tomonori Usuda"
  ],
  "comment": "15 pages, 8 figures, and 1 table, accepted for publication in ApJ",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "We present measurements of the clustering properties of a sample of infrared (IR) bright dust-obscured galaxies (DOGs). Combining 125 deg$^2$ of wide and deep optical images obtained with the Hyper Suprime-Cam on the Subaru Telescope and all-sky mid-IR (MIR) images taken with Wide-Field Infrared Survey Explorer, we have discovered 4,367 IR-bright DOGs with $(i - [22])_{\\rm AB}$ $>$ 7.0 and flux density at 22 $\\mu$m $>$ 1.0 mJy. We calculate the angular autocorrelation function (ACF) for a uniform subsample of 1411 DOGs with 3.0 mJy $<$ flux (22 $mu$m) $<$ 5.0 mJy and $i_{\\rm AB}$ $<$ 24.0. The ACF of our DOG subsample is well-fit with a single power-law, $\\omega (\\theta)$ = (0.010 $\\pm$ 0.003) $\\theta^{-0.9}$, where $\\theta$ in degrees. The correlation amplitude of IR-bright DOGs is larger than that of IR-faint DOGs, which reflects a flux-dependence of the DOG clustering, as suggested by Brodwin et al. (2008). We assume that the redshift distribution for our DOG sample is Gaussian, and consider 2 cases: (1) the redshift distribution is the same as IR-faint DOGs with flux at 22 $\\mu$m $<$ 1.0 mJy, mean and sigma $z$ = 1.99 $\\pm$ 0.45, and (2) $z$ = 1.19 $\\pm$ 0.30, as inferred from their photometric redshifts. The inferred correlation length of IR-bright DOGs is $r_0$ = 12.0 $\\pm$ 2.0 and 10.3 $\\pm$ 1.7 $h^{-1}$ Mpc, respectively. IR-bright DOGs reside in massive dark matter halos with a mass of $\\log [\\langle M_{\\mathrm{h}} \\rangle / (h^{-1} M_{\\odot})]$ = 13.57$_{-0.55}^{+0.50}$ and 13.65$_{-0.52}^{+0.45}$ in the two cases, respectively.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2016-12-04T09:10:07.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "infrared-bright dust-obscured galaxies",
      "hyper suprime-cam",
      "ir-faint dogs",
      "redshift distribution",
      "clustering"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 15,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}