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We study the angular correlation function of star-forming galaxies andproperties 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 respectivelycover large angular areas of 16.3 deg^2 and 16.9 deg^2. Our sample contains8302 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 thecorrelation from a simple power-law form. To interpret the measured clusteringsignal, we adopt a halo occupation distribution (HOD) model that is constructedto explain the spatial distribution of galaxies selected by a star formationrate. The observed correlation function and number density are simultaneouslyexplained by the best-fitting HOD model. From the constrained HOD model, theaverage 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 becomehalos with the present-day mass, $M\sim 1.5 \times 10^{13}h^{-1}M_\odot$. Thesatellite fraction of the [OII] emitter sample is found to be $f_{sat}\sim0.15$. All these values are consistent with the previous studies of similarsamples, but we obtain tighter constraints even in a larger parameter space dueto 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 catalogsand the systematic forecast study of cosmological constraints from upcomingemission line galaxy surveys such as the Subaru PFS survey.

Angular clustering and host halo properties of [OII] emitters at $z >1$ in the Subaru HSC survey