z=0.1 ~ 0.9团簇中热等离子体与Galerkin相互作用的探讨
Probing of the Interactions Between the Hot Plasmas and Galaxies in Clusters from z=0.1 to 0.9
摘要：
根据34个红移为0.1-0.9的弛豫富星系团的光学和X射线数据，研究了团星系和热等离子体两种主要重子含量的相对空间分布。使用UH 88望远镜拍摄的多波段光度数据，我们使用两种独立的方法确定了每个星系团中成员星系的综合（二维）径向光剖面，即，背景减除和颜色幅度滤波。ICM质量分布的每个集群在我们的样品中，也集成在两个维度上，来自空间分辨光谱分析使用XMM牛顿和钱德拉数据。然后，每个星系团的径向积分光分布除以其ICM质量分布，以获得“星系光与ICM质量比”的分布。发现在中心0.65 R500区域的比率分布从高红移到低红移的子样本变陡，这意味着星系在ICM球中变得更加集中，朝向较低的红移。这种演化也可以在星系数与ICM质量比的曲线中看到。已经评估了星系光测量中的一系列系统不确定性，以及星系与ICM轮廓的许多半径/红移依赖性偏差，但它们都不显著。此外，星系光与总质量比的分布也呈现出向低红移方向逐渐集中的趋势。我们解释的背景下，星系，ICM，和暗物质组件遵循类似的空间分布在早期阶段（z>0.5），而星系已下降到中心相对于其他在较晚的阶段。
英文摘要：
Based on optical and X-ray data for a sample of 34 relaxed rich clusters of galaxies with redshifts of 0.1-0.9, we studied relative spatial distributions of the two major baryon contents, the cluster galaxies and the hot plasmas. Using multi-band photometric data taken with the UH88 telescope, we determined the integrated (two dimensional) radial light profiles of member galaxies in each cluster using two independent approaches, i.e., the background subtraction and the color-magnitude filtering. The ICM mass profile of each cluster in our sample, also integrated in two dimensions, was derived from a spatially-resolved spectral analysis using XMM-Newton and Chandra data. Then, the radially-integrated light profile of each cluster was divided by its ICM mass profile, to obtain a profile of "galaxy light vs. ICM mass ratio". The ratio profiles over the central 0.65 R500 regions were found to steepen from the higher- to lower- redshift subsamples, meaning that the galaxies become more concentrated in the ICM sphere towards lower redshifts. The evolution is also seen in galaxy number vs. ICM mass ratio profiles. A range of systematic uncertainties in the galaxy light measurements, as well as many radius-/redshift- dependent biases to the galaxy vs. ICM profiles have been assessed, but none of them is significant against the observed evolution. Besides, the galaxy light vs. total mass ratio profiles also exhibit gradual concentration towards lower redshift. We interpret in the context that the galaxies, the ICM, and the dark matter components followed a similar spatial distribution in the early phase (z>0.5), while the galaxies have fallen towards the center relative to the others at a later phase.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
