揭开武仙座超星系团的内部结构
Unveiling the internal structure of Hercules supercluster
摘要：
我们已经调查了武仙座超星系团（SCL 160）的结构的基础上，最初从斯隆数字巡天SDSS-DR 7提取的数据。我们通过星系的$r^\prime$光度加权的数值密度追踪了场中的质量分布，并根据它们的空间位置和红移对它们进行了分类。这使我们不仅能够解决整个超星系团的运动学，而且还解决了每个星系团的内部运动学，这是以前没有进一步探索过的。我们已经证实武仙座超星系团是由星系团A2147、A2151和A2152组成的。A2151由五个子星系团组成，A2147在两个，A2152至少在两个。它们是武仙座超星系团的核心。我们还发现了另外两个引力键星系团，因此增加了超星系团的已知成员。我们估计武仙座超星系团的总质量为$2.1\pm0.2 \times 10^{15}$ M $_\odot$。为了确定动力学质量，在这项工作中，我们采取了$M_{200}-σ$标度关系和焦散技术。将这两种方法与双峰合并集群的模拟数据进行比较，我们发现焦散以及基于$σ$的质量在合并年龄期间存在偏差，在臂间通道之后显示出提升。这不符合焦散方法的原则，即它不依赖于团簇的动力学状态。
英文摘要：
We have investigated the structure of the Hercules supercluster (SCL160) based on data originally extracted from the Sloan Digital Sky Survey SDSS-DR7. We have traced the mass distribution in the field through the numerical density-weighted by the $r^\prime$-luminosity of the galaxies and classified them based on their spatial position and redshift. This has allowed us not only to address the kinematics of the supercluster as a whole, but also the internal kinematic of each cluster, which was no further explored before. We have confirmed that the Hercules supercluster is composed of the galaxy clusters A2147, A2151, and A2152. A2151 consists of five subclusters, A2147 on two and A2152 on at least two. They form the heart of the Hercules supercluster. We also have found two other gravitationally bond clusters, increasing, therefore, the known members of the supercluster. We have estimated a total mass of $2.1\pm0.2 \times 10^{15}$ M$_\odot$ for the Hercules supercluster. To determine the dynamical masses in this work, we have resorted to the $M_{200}-σ$ scaling relation and the caustic technique. Comparing both methods with simulated data of bimodal merging clusters, we found the caustic, as well as the $σ$-based masses, are biased through the merger age, showing a boost just after the pericentric passage. This is not in line with the principle of the caustic method that affirms it is not depending on the cluster dynamical state.
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