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 KomiyamaSatoshi Miyazaki, Akatoki Noboriguchi, Tomonori Usuda

Research output: Contribution to journalArticlepeer-review

21 Scopus citations


We present measurements of the clustering properties of a sample of infrared (IR) bright dust-obscured galaxies (DOGs). Combining 125 deg2 of wide and deep optical images obtained with the Hyper Suprime-Cam on the Subaru Telescope and all-sky mid-IR images taken with Wide-Field Infrared Survey Explorer, we have discovered 4367 IR-bright DOGs with and flux density at 22 mJy. We calculate the angular autocorrelation function (ACF) for a uniform subsample of 1411 DOGs with 3.0 mJy < flux (22 ) < 5.0 mJy and < 24.0. The ACF of our DOG subsample is well-fit with a single power law, ω(θ)=(0.010 ± 0.003) , where θ is 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. We assume that the redshift distribution for our DOG sample is Gaussian, and consider two cases: (1) the redshift distribution is the same as IR-faint DOGs with flux at 22 < 1.0 mJy, mean and sigma z = 1.99 ±0.45, and (2) z = 1.19 ±0.30, as inferred from their photometric redshifts. The inferred correlation length of IR-bright DOGs is r 0 = 12.0 ±2.0 and 10.3 ±1.7 Mpc, respectively. IR-bright DOGs reside in massive dark matter halos with a mass of log[〈Mh〉 /(h-1M⊙)]13.57-0.55 +0.50 and 13.65+0.45 -0.52 in the two cases, respectively.

Original languageEnglish (US)
Article number36
JournalAstrophysical Journal
Issue number1
StatePublished - Jan 20 2017

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


  • catalogs
  • galaxies: active
  • infrared: galaxies
  • methods: statistical

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