在暗物质模拟中“观测”非弛豫星系团
"Observing" Unrelaxed Clusters in Dark Matter Simulations
摘要：
我们提出了一个详细的研究放松和非放松的星系团在一个大的暗物质模拟。最近的工作已经证明了具有高斯速度分布（放松）的星系团与不具有高斯速度分布（非放松）的星系团之间的明显差异。为了直接与观测结果进行比较，我们使用一维速度分布识别模拟中的非松弛簇。我们发现，非高斯星系团有最近的主要合并和增强率的星系相对于系统的高斯速度分布。此外，我们发现非高斯团簇的比例随着团簇质量的增加而强烈增加，随着红移的增加而适度增加。为了比较，我们还利用模拟中的三维信息来探索投影对观测测量的影响。当考虑三维信息时，高斯和非高斯集群之间的差异要大得多，这表明观察到的集群动态趋势的强度被观察到的速度信息限制在一条视线内所稀释。
英文摘要：
We present a detailed study of relaxed and unrelaxed galaxy clusters in a large dark-matter only simulation. Recent work has demonstrated clear differences between the galaxy populations in clusters which have Gaussian velocity distributions (relaxed) compared to those that do not (unrelaxed). To directly compare with observations, we identify unrelaxed clusters in the simulations using one-dimensional velocity distributions. We show that non-Gaussian clusters have had recent major mergers and enhanced rates of galaxy infall relative to systems with Gaussian velocity profiles. Furthermore, we find that the fraction of non-Gaussian clusters increases strongly with cluster mass and modestly with redshift. For comparison, we also make use of three-dimensional information available in the simulations to explore the impact of projection on observational measurements. Differences between Gaussian and non-Gaussian clusters are much stronger when three-dimensional information is considered, which demonstrates that the strength of observed trends with cluster dynamics are diluted by observed velocity information being limited to one line-of-sight.
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