2016/12/04 by Yoshiki Toba, Tohru Nagao, Masaru Kajisawa +20 · 1 citation
Physics and Astronomy · #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.3847/1538-4357/835/1/36
15 pages, 8 figures, and 1 table, accepted for publication in ApJ
arxiv created 2016/12/04 · arxiv updated 2017/01/25
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 (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 μm > 1.0 mJy. We calculate the angular autocorrelation function (ACF) for a uniform subsample of 1411 DOGs with 3.0 mJy < flux (22 mum) < 5.0 mJy and i\rm AB < 24.0. The ACF of our DOG subsample is well-fit with a single power-law, ω(θ) = (0.010 ± 0.003) θ-0.9, where θ 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 μm < 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 r0 = 12.0 ± 2.0 and 10.3 ± 1.7 h-1 Mpc, respectively. IR-bright DOGs reside in massive dark matter halos with a mass of log [⟨ Mh ⟩ / (h-1 M\odot)] = 13.57-0.55+0.50 and 13.65-0.52+0.45 in the two cases, respectively.