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) Subaru Stragetic Program (SSP) survey. We use [O ii] 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 deg2 and 16.9 deg2. Our sample contains 8302 and 9578 [O ii] emitters at z = 1.19 (NB816) and z = 1.47 (NB921), respectively. We detect a strong clustering signal over a wide angular range, $0{_{.}^{\circ}} 001$ < θ < 1 °, with 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 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 [O ii] emitters is derived to be $\log {M_{\rm eff}/(h^{-1}\, {M}_{\odot })}=12.70^{+0.09}_{-0.07}$ 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 ∼ 1.5 × 1013 h−1 M⊙. The satellite fraction of the [O ii] emitter sample is found to be fsat ∼ 0.15. All these values are consistent with 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 [O ii] 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 Prime Focus Spectrograph survey.

中文翻译：

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斯巴鲁 HSC 调查中 z > 1 处 [O ii] 发射器的角聚类和主晕特性

我们研究了恒星形成星系的角相关函数及其宿主暗物质晕在 z > 处的性质。1 使用 Hyper-Suprime Cam (HSC) 斯巴鲁战略计划 (SSP) 调查。我们使用在 Deep/UltraDeep 层中使用两个窄带 (NB) 滤波器 NB816 和 NB921 识别的 [O ii] 发射器，它们分别覆盖 16.3 deg2 和 16.9 deg2 的大角度区域。我们的样品分别在 z = 1.19 (NB816) 和 z = 1.47 (NB921) 处包含 8302 和 9578 个 [O ii] 发射器。我们在很宽的角度范围内检测到强聚类信号 $0{_{.}^{\circ}} 001$ < θ＜1°，偏置 $b=1.61^{+0.13}_{-0.11}$ (z = 1.19) 和 $b=2.09^{+0.17}_{-0.15}$ (z = 1.47)。我们还发现相关性与简单的幂律形式存在明显偏差。为了解释测量的聚类信号，我们采用光晕占据分布（HOD）模型来解释由恒星形成率选择的星系的空间分布。观察到的相关函数和数密度由最佳拟合 HOD 模型同时解释。从受约束的 HOD 模型中，托管 [O ii] 发射器的光晕的平均质量导出为 $\log {M_{\rm eff}/(h^{-1}\, {M}_{\odot } )}=12.70^{+0.09}_{-0.07}$ 和 $12.61^{+0.09}_{-0.05}$ 分别在 z = 1.19 和 1.47 处，它们将成为当前质量 M ∼ 1.5 的光晕× 1013 h−1 M⊙。发现 [O ii] 发射器样本的卫星分数为 fsat ∼ 0.15。所有这些值都与先前对类似样本的研究一致，但由于来自 HSC 的样本量更大，即使在更大的参数空间中，我们也获得了更严格的约束。