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arXiv 2103.08628astro-ph.GAastro-ph.CO
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斯巴鲁超级超级凸轮巡天$0.10 \leq z \leq 1.05$测光亮红星系成团的晕模型分析

Halo-model analysis of the clustering of photometric luminous red galaxies at $0.10 \leq z \leq 1.05$ from the Subaru Hyper Suprime-Cam Survey

Shogo Ishikawa, Teppei Okumura, Masamune Oguri, Sheng-Chieh Lin

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16 pages, 7 figures, 2 tables, accepted for publication in ApJ
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摘要：

我们提出的光度发光的红色星系（LRGs）的聚类分析的红移范围为$0.1\leq z \leq 1.05$使用$615,317$光度LRGs选择的超级Suprime-Cam斯巴鲁战略计划涵盖$\sim124$度$^{2}$。我们的样本涵盖了广泛的恒星质量和光度红移，并使晕占据分布分析，研究红移和恒星质量的依赖性的暗晕性质的LRGs。我们发现一个紧密的相关性之间的特征暗晕质量主机中央LRGs，$M_{\min}$，和独立的红移LRGs的数密度，表明LRGs的形成与全球环境。LRG的$M_{\min}$仅弱依赖于恒星质量$M_{\star}$在$M_{\star} \lesssim 10^{10.75}h^{-2} M_{\odot}$在$0.3<z<1.05$，在对比的情况下，所有光度选择的星系，$M_{\min}$显示出显着的依赖于$M_{\star}$，即使在低$M_{\star}$。弱的恒星质量依赖性表明暗晕质量是LRG形成的关键参数，而不是恒星质量。我们的结果表明，由于晕环境，$\sim 10^{12.5 \pm 0.2}h^{-1} M_{\odot}$的晕质量是有效晕淬灭的临界质量。通过与流体动力学模拟结果的比较发现，$z \sim 1$低质量LRGs通过合并和卫星吸积将使它们的恒星质量从$z=1$增加到$0$一个数量级，而$z<0.9$大质量LRGs中有很大一部分是最近从大质量绿谷星系迁移过来的LRGs，或者是通过合并和卫星吸积从质量较小的LRGs演化而来的LRGs.

英文摘要：

We present the clustering analysis of photometric luminous red galaxies (LRGs) at a redshift range of $0.1\leq z \leq 1.05$ using $615,317$ photometric LRGs selected from the Hyper Suprime-Cam Subaru Strategic Program covering $\sim124$ deg$^{2}$. Our sample covers a broad range of stellar masses and photometric redshifts and enables a halo occupation distribution analysis to study the redshift and stellar-mass dependence of dark halo properties of LRGs. We find a tight correlation between the characteristic dark halo mass to host central LRGs, $M_{\min}$, and the number density of LRGs independently of redshifts, indicating that the formation of LRGs is associated with the global environment. The $M_{\min}$ of LRGs depends only weakly on the stellar mass $M_{\star}$ at $M_{\star} \lesssim 10^{10.75}h^{-2} M_{\odot}$ at $0.3<z<1.05$, in contrast to the case for all photometrically selected galaxies for which $M_{\min}$ shows significant dependence on $M_{\star}$ even at low $M_{\star}$. The weak stellar mass dependence is indicative of the dark halo mass being the key parameter for the formation of LRGs rather than the stellar mass. Our result suggests that the halo mass of $\sim 10^{12.5 \pm 0.2}h^{-1} M_{\odot}$ is the critical mass for an efficient halo quenching due to the halo environment. We compare our result with the result of the hydrodynamical simulation to find that low-mass LRGs at $z \sim 1$ will increase their stellar masses by an order magnitude from $z=1$ to $0$ through mergers and satellite accretions, and a large fraction of massive LRGs at $z<0.9$ consist of LRGs that are recently migrated from massive green valley galaxies or those evolved from less massive LRGs through mergers and satellite accretions.

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