浓度是否会驱动星系团恒星与晕质量关系中的散射？
Does Concentration Drive the Scatter in the Stellar-to-Halo Mass Relation of Galaxy Clusters?
摘要：
浓度是暗物质晕的关键属性之一，它可以驱动大质量星系团的恒星-晕质量关系中的散射。我们得到了强大的光度恒星质量的样本中最亮的中央星系（BCGs）的SDSS redMapper集群在$0.17<z<0.3$，并分裂成两个相等的晕质量的子样本的星团由他们的BCG恒星质量$M_*$。弱透镜配置文件$ΔΣ$的两个集群子样本表现出不同的斜率尺度低于1 M $pc/h$。为了解释这种差异，我们进行了一个全面的贝叶斯模型的两个$ΔΣ$配置文件，包括不同程度的偏心效应之间的两个子样本的X射线观测。发现两个子样品具有相同的平均晕质量$1.74 \times 10^{14} M_{\odot}/h$，但低$M_*$团簇的浓度为$5.87_{-0.60}^{+0.77}$，${\sim}1.5σ$小于高$M_*$团簇的浓度~（$6.95_{-0.66}^{+0.78}$）.此外，星系团弱透镜效应和星系团-星系的互相关都表明，低$M_*$、低浓度星系团的大尺度偏置比高$M_*$、高浓度星系团的大尺度偏置高${\sim}10\%$，这可能是星系团组装偏置效应的证据。我们的研究结果揭示了一个显着的物理联系的恒星质量在20{-}30 k $pc/h$，暗物质质量在${\sim}$ 200 k $pc/h$，和宇宙的超密度在10 M以上的尺度$pc/h$，使一个关键的观测测试的大质量星系团和它们的中央星系之间的共同演化的理论。
英文摘要：
Concentration is one of the key dark matter halo properties that could drive the scatter in the stellar-to-halo mass relation of massive clusters. We derive robust photometric stellar masses for a sample of brightest central galaxies (BCGs) in SDSS redMaPPer clusters at $0.17<z<0.3$, and split the clusters into two equal-halo mass subsamples by their BCG stellar mass $M_*$. The weak lensing profiles $ΔΣ$ of the two cluster subsamples exhibit different slopes on scales below 1 M$pc/h$. To interpret such discrepancy, we perform a comprehensive Bayesian modelling of the two $ΔΣ$ profiles by including different levels of miscentring effects between the two subsamples as informed by X-ray observations. We find that the two subsamples have the same average halo mass of $1.74 \times 10^{14} M_{\odot}/h$, but the concentration of the low-$M_*$ clusters is $5.87_{-0.60}^{+0.77}$, ${\sim}1.5σ$ smaller than that of their high-$M_*$ counterparts~($6.95_{-0.66}^{+0.78}$). Furthermore, both cluster weak lensing and cluster-galaxy cross-correlations indicate that the large-scale bias of the low-$M_*$, low-concentration clusters are ${\sim}10\%$ higher than that of the high-$M_*$, high-concentration systems, hence possible evidence of the cluster assembly bias effect. Our results reveal a remarkable physical connection between the stellar mass within 20{-}30 k$pc/h$, the dark matter mass within ${\sim}$ 200 k$pc/h$, and the cosmic overdensity on scales above 10 M$pc/h$, enabling a key observational test of theories of co-evolution between massive clusters and their central galaxies.
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