SDSS中的NoSOCS。I.样本定义和质量估计值的比较
NoSOCS in SDSS. I. Sample Definition and Comparison of Mass Estimates
摘要：
我们使用斯隆数字巡天（SDSS）的数据，调查星系团的性质的系统内首次发现DPOSS。利用SDSS的高质量测光结果，我们导出了新的测光红移，并估算了丰度和光学光度。对于低红移（$z \le 0.1$）集群的一个子集，我们已经使用SDSS光谱数据，以确定在红移空间中的每个集群的区域中的组，从文献中的大规模系统的补充，以确保连续的质量采样。一种方法，以消除闯入者的应用，并进行维里分析，从而估计速度分散，质量，和物理半径为每个低$z$系统。我们讨论了选择的最大半径和光度范围的动力学分析，表明光谱调查必须完成至少M $^*+1$，如果一个希望获得准确和公正的估计速度色散和质量。我们已经测量了X射线光度的所有集群使用档案数据从RASS。对于一个较小的子集（21个集群），我们从文献中选择的温度措施和估计质量的M-T $_X$关系，发现他们表现出良好的协议与维里估计。然而，这两个质量估计值往往与焦散结果不一致。我们测量了样品中所有簇的亚结构的存在，发现具有亚结构的簇的维里质量高于来自T $_X$的那些。当比较焦散和X射线质量时，未观察到这种趋势。这是因为焦散质量是直接从质量剖面估算的，所以它受子结构的影响较小。
英文摘要：
We use Sloan Digital Sky Survey (SDSS) data to investigate galaxy cluster properties of systems first detected within DPOSS. With the high quality photometry of SDSS we derived new photometric redshifts and estimated richness and optical luminosity. For a subset of low redshift ($z \le 0.1$) clusters, we have used SDSS spectroscopic data to identify groups in redshift space in the region of each cluster, complemented with massive systems from the literature to assure the continuous mass sampling. A method to remove interlopers is applied, and a virial analysis is performed resulting in estimates of velocity dispersion, mass, and a physical radius for each low-$z$ system. We discuss the choice of maximum radius and luminosity range in the dynamical analysis, showing that a spectroscopic survey must be complete to at least M$^*+1$ if one wishes to obtain accurate and unbiased estimates of velocity dispersion and mass. We have measured X-ray luminosity for all clusters using archival data from RASS. For a smaller subset (twenty-one clusters) we selected temperature measures from the literature and estimated mass from the M-T$_X$ relation, finding that they show good agreement with the virial estimate. However, these two mass estimates tend to disagree with the caustic results. We measured the presence of substructure in all clusters of the sample and found that clusters with substructure have virial masses higher than those derived from T$_X$. This trend is not seen when comparing the caustic and X-ray masses. That happens because the caustic mass is estimated directly from the mass profile, so it is less affected by substructure.
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