Clustering of infrared-bright dust-obscured galaxies revealed by the
  Hyper Suprime-Cam and WISE
  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.
