Angular clustering and host halo properties of [OII] emitters at $z >1$
  in the Subaru HSC survey
  We study the angular correlation function of star-forming galaxies and
properties of their host dark matter halos at z>1 using the Hyper-Suprime Cam
(HSC) SSP survey. We use [OII] emitters identified using two narrow-band (NB)
filters, NB816 and NB921, in the Deep/UltraDeep layers, which respectively
cover large angular areas of 16.3 deg^2 and 16.9 deg^2. Our sample contains
8302 and 9578 [OII] emitters at z=1.19 (NB816) and z=1.47 (NB921),
respectively. We detect a strong clustering signal over a wide angular range,
0.001 < \theta < 1 [deg], with the bias $b=1.61^{+0.13}_{-0.11}$ (z=1.19) and
$b=2.09^{+0.17}_{-0.15}$ (z=1.47). We also find a clear deviation of the
correlation from a simple power-law form. To interpret the measured clustering
signal, we adopt a halo occupation distribution (HOD) model that is constructed
to explain the spatial distribution of galaxies selected by a star formation
rate. The observed correlation function and number density are simultaneously
explained by the best-fitting HOD model. From the constrained HOD model, the
average mass of halos hosting the [OII] emitters is derived to be
$\log{M_{eff}/(h^{-1}M_\odot)}=12.70^{+0.09}_{-0.07}$ and
$12.61^{+0.09}_{-0.05}$ at z=1.19 and 1.47, respectively, which will become
halos with the present-day mass, $M\sim 1.5 \times 10^{13}h^{-1}M_\odot$. The
satellite fraction of the [OII] emitter sample is found to be $f_{sat}\sim
0.15$. All these values are consistent with the previous studies of similar
samples, but we obtain tighter constraints even in a larger parameter space due
to the larger sample size from the HSC. The results obtained for host halos of
[OII] emitters in this paper enable the construction of mock galaxy catalogs
and the systematic forecast study of cosmological constraints from upcoming
emission line galaxy surveys such as the Subaru PFS survey.
