8个富星系团的视向速度成员研究

Studies of Radial Velocity Members for Eight Rich Galaxy Clusters

本文利用在考虑团内星系面数密度分布的前提下，以视向速度为判据，按最大似然原理解算团分布参数和成员概率的严格统计方法，对8个Abell星系团进行了成员研究．解算结果表明此方法是合理的、有效的，星系团的速度弥散度分布与动力学模型一致．有迹象表明椭长形的结构在星系团中是一种普遍现象．从这8个团得到了清晰的NA－σc的相关关系，进而推知团的质光比为100～600h，平均350h．

On the basis of radial velocity membership determination method, while the distribution of surface-number-density of galaxies in cluster regions is concerned s imultaneously, we calculate the distribution parameters and membership probabilities of individual galaxies for 8 Abell clusters. It is shown that the membership determination approach is a reasonable and feasible one, and distributions of radial velocity dispersions of these clusters are in agreement with the dynamical model. Elongate structures seem to be a universal appearance for rich galaxy clusters. From these 8 clusters, we have found an obvious relationship between NA and σc of galaxy clusters, and furthermore, inferred that the Mass to Luminosity Ratio of rich galaxy clusters are from 100 to 600h, with the average value being 350 h.