论文标题
Chandra X射线群集样品的暗物质核心密度和半径的缩放关系
Scaling relations for dark matter core density and radius from Chandra X-ray cluster sample
论文作者
论文摘要
大量研究发现，暗物质核心半径（$ r_c $）和核心密度（$ρ_C$）给出的暗物质表面密度大约在各种星系系统的范围内恒定。但是，对于Chan（Arxiv：1403.4352）的Galaxy Clusters的该{\ IT ANSATZ}只有一项系统的研究，他们发现簇的表面密度不是恒定的，$ρ_C\ sim r_c \ sim r_c^r_c^{ - 1.46} $。我们对Chandra观察结果的12个放松簇的X射线样本进行了此测试，实施了与Chan相同的程序，但也考虑了气体和星形质量。我们发现$ρ_C\ propto r_c^{ - 1.08 \ pm 0.055} $，内在散布约为18％。因此，我们的群集数据的暗物质表面密度显示出与仅约1.4 $σ$的恒定值的偏差。
A large number of studies have found that the dark matter surface density, given by the product of the dark matter core radius ($r_c$) and core density ($ρ_c$) is approximately constant for a wide range of galaxy systems. However, there has been only one systematic study of this {\it ansatz} for galaxy clusters by Chan (arXiv:1403.4352), who found that the surface density for clusters is not constant and $ρ_c \sim r_c^{-1.46}$. We carry out this test for an X-ray sample of 12 relaxed clusters from Chandra observations, implementing the same procedure as Chan, but also accounting for the gas and star mass. We find that $ρ_c \propto r_c^{-1.08 \pm 0.055}$, with an intrinsic scatter of about 18%. Therefore, the dark matter surface density for our cluster data shows deviations from a constant value at only about 1.4$σ$.
