HSC-XXL: Baryon budget of the 136 XXL groups and clusters
HSC-XXL: Baryon budget of the 136 XXL groups and clusters
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DOI：
10.1093/pasj/psab115
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发表时间：
2022-02-01
影响因子：
2.3
通讯作者：
Tanaka, Masayuki
中科院分区：
文献类型：
--
作者：
Akino, Daichi;Eckert, Dominique;Tanaka, Masayuki
我们给出了我们对X射线选择的XXL样本的重子预算的测定，该样本包含136个星系群和星系团，它们的质量跨越近两个数量级（M-500类似于10（13）-10（15）M-圆点），红移范围0小于或类似于z小于或类似于1。我们的联合分析是基于Hyper Suprime-Cam Subaru战略计划（HSC-SSP）弱透镜质量测量，XXL X射线气体质量测量以及HSC和Sloan数字巡天多波段测光的组合。我们进行了贝叶斯分析的多元质量标度关系的气体质量，星系恒星质量，恒星质量的最亮的星系团（BCGs），和软带X射线光度，考虑到集群属性，选择效应，弱透镜质量校准之间的内在协方差，观测误差协方差矩阵。气体质量-总质量（M-500）关系的质量相关斜率为1.29（-0.10）（+0.16），比自相似预测的单位质量更陡，而恒星质量-总质量关系的斜率比单位质量更浅：0.85（-0.09）（+0.12）。BCG恒星质量与星团质量的关系很弱，斜率为0.49（-0.10）（+0.11）。重子，气体质量和恒星质量分数作为M-500的函数，同意从数值模拟和以前的观测结果。我们成功地约束重子内容的全部内在协方差。BCG的恒星质量显示较大的内在散射在一个给定的晕总质量，其次是恒星质量和气体质量。我们发现一个显着的正的内在相关系数之间的总（和卫星）恒星质量和BCG恒星质量和气体质量和恒星质量之间的内在相关性没有证据。所有重子分量都没有表现出红移演化。
We present our determination of the baryon budget for an X-ray-selected XXL sample of 136 galaxy groups and clusters spanning nearly two orders of magnitude in mass (M-500 similar to 10(13)-10(15) M-circle dot) and the redshift range 0 less than or similar to z less than or similar to 1. Our joint analysis is based on the combination of Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) weak-lensing mass measurements, XXL X-ray gas mass measurements, and HSC and Sloan Digital Sky Survey multiband photometry. We carry out a Bayesian analysis of multivariate mass-scaling relations of gas mass, galaxy stellar mass, stellar mass of brightest cluster galaxies (BCGs), and soft-band X-ray luminosity, by taking into account the intrinsic covariance between cluster properties, selection effect, weak-lensing mass calibration, and observational error covariance matrix. The mass-dependent slope of the gas mass-total mass (M-500) relation is found to be 1.29(-0.10)(+0.16), which is steeper than the self-similar prediction of unity, whereas the slope of the stellar mass-total mass relation is shallower than unity; 0.85(-0.09)(+0.12). The BCG stellar mass weakly depends on cluster mass with a slope of 0.49(-0.10)(+0.11). The baryon, gas mass, and stellar mass fractions as a function of M-500 agree with the results from numerical simulations and previous observations. We successfully constrain the full intrinsic covariance of the baryonic contents. The BCG stellar mass shows the larger intrinsic scatter at a given halo total mass, followed in order by stellar mass and gas mass. We find a significant positive intrinsic correlation coefficient between total (and satellite) stellar mass and BCG stellar mass and no evidence for intrinsic correlation between gas mass and stellar mass. All the baryonic components show no redshift evolution.