z ~ 0.9的合并超星系团RCS 231953+00的结构
The structure of the merging RCS 231953+00 Supercluster at z ~ 0.9
摘要：
RCS 2319+00超星系团是一个z=0.9的大质量超星系团，由三个光学选择的、光谱确认的星系团组成，在天球平面上的距离小于3 Mpc。这个超星系团是现今大质量星系团（10^{15} Msun x z~0.5）的几个已知祖先之一。我们提出了一个广泛的光谱运动进行的超星系团领域的结果，结合以前公布的数据，在1961年高置信度星系红移。我们发现302个结构成员跨越三个不同的红移墙彼此分开约65 Mpc。组成团簇的光谱红移分别为0.901、0.905和0.905。速度色散与X射线数据预测的结果一致，给出的星团质量估计为~10^{14.5} - 10^{14.9} Msun。Dressler-Shectman测试发现了超星系团场的子结构证据，朋友的朋友分析确定了超星系团中的5个群体，包括Coppin等人（2012）先前在红外线中确定的两个星系团核心之间的延伸结构。星系的颜色进一步显示这个星系结构是超星系团中一个独特的活动区域，主要由蓝色星系组成，而其他星系团和星系团核心中的红色序列星系约占43-77%。根据叠加光度函数拟合得到的丰度估计值与平均群质量估计值一致，约为10^{13} Msun晕。目前，我们确认的成员中有22%居住在>~10^{13} Msun的星系群/星系团中，这些星系团/星系团注定要合并到最大质量的星系团中，这与N体模拟合并树研究中星系团预处理中重要的大质量晕星系分数一致。
英文摘要：
The RCS 2319+00 supercluster is a massive supercluster at z=0.9 comprising three optically selected, spectroscopically confirmed clusters separated by <3 Mpc on the plane of the sky. This supercluster is one of a few known examples of the progenitors of present-day massive clusters (10^{15} Msun by z~0.5). We present an extensive spectroscopic campaign carried out on the supercluster field resulting, in conjunction with previously published data, in 1961 high confidence galaxy redshifts. We find 302 structure members spanning three distinct redshift walls separated from one another by ~65 Mpc. The component clusters have spectroscopic redshifts of 0.901, 0.905 and 0.905. The velocity dispersions are consistent with those predicted from X-ray data, giving estimated cluster masses of ~10^{14.5} - 10^{14.9} Msun. The Dressler-Shectman test finds evidence of substructure in the supercluster field and a friends-of-friends analysis identified 5 groups in the supercluster, including a filamentary structure stretching between two cluster cores previously identified in the infrared by Coppin et al. (2012). The galaxy colors further show this filamentary structure to be a unique region of activity within the supercluster, comprised mainly of blue galaxies compared to the ~43-77% red-sequence galaxies present in the other groups and cluster cores. Richness estimates from stacked luminosity function fits results in average group mass estimates consistent with ~10^{13} Msun halos. Currently, 22% of our confirmed members reside in >~10^{13} Msun groups/clusters destined to merge onto the most massive cluster, in agreement with the massive halo galaxy fractions important in cluster galaxy pre-processing in N-body simulation merger tree studies.
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