论文标题
[OII]发射器的角簇和主机光环属性在Subaru HSC调查中$ z> 1 $
Angular clustering and host halo properties of [OII] emitters at $z >1$ in the Subaru HSC survey
论文作者
论文摘要
我们使用Hyper-Suprime CAM（HSC）SSP调查研究了恒星形成星系的角度相关函数及其宿主暗物质光环的特性。我们在深度/超过的层中使用了使用两个窄带（NB）滤波器NB816和NB921鉴定的[OII]发射器，它们分别覆盖了16.3 ver^2和16.9 veg^2的大型角区域。我们的样本分别包含8302和9578 [OII] Z = 1.19（NB816）和Z = 1.47（NB921）的发射器。我们在宽角度范围内检测到一个强的聚类信号，0.001 <θ<1 [deg]，偏见$ b = 1.61^{+0.13} _ { - 0.11} $（z = 1.19）和$ b = 2.09^{+0.17} {+0.17} _ { - 0.15} _ { - 0.15} $（z = 1.47）。我们还发现与简单的幂律形式的相关性明显偏差。为了解释测得的聚类信号，我们采用了一个光晕占用分布（HOD）模型，该模型的构建是为了解释由恒星形成速率选择的星系的空间分布。观察到的相关函数和数量密度通过最合适的HOD模型同时解释。从受约束的HOD模型中，托管[OII]发射器的平均质量被得出为$ \ log {m_ {eff}/（h^{ - 1} m_ \ odot）} = 12.70^{+0.09} _ {+0.09} _ { - 0.09} _ { - 0.07} $ and $ 12.61 $ and $ 12.61^$ an z = 1.19和1.47，分别将变成现有质量的晕子，$ m \ sim 1.5 \ times 10^{13} h^{ - 1} m_ \ odot $。发现[OII]发射极样本的卫星分数为$ f_ {sat} \ sim 0.15 $。所有这些值都与以前对相似样品的研究一致，但是由于HSC的样本量较大，我们即使在较大的参数空间中也获得了更严格的约束。本文中[OII]发射器的宿主光环获得的结果使模拟星系目录的构建以及从即将到来的发射线星系调查（例如Subaru PFS调查）对宇宙学约束的系统预测研究。
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 < θ< 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.
