星系团数值模拟中扩散物质的相干旋转
On the coherent rotation of diffuse matter in numerical simulations of galaxy clusters
摘要：
我们提出了一个研究的相干旋转的集群内的介质和暗物质成分的模拟星系团提取的体积有限的样本的MUSIC项目。用三种不同的气体物理方案重新模拟了该集合：$(i)$无辐射方案、$(ii)$无活动星系核反馈辐射方案和$(iii)$有活动星系核反馈辐射方案。我们的分析是基于146个被确定为放松的最大集群，占总样本的57%。我们将这些物体分为旋转和非旋转的气体自旋参数，一个数量，可以与集群的意见。我们发现，4%的放松样本旋转根据我们的标准。通过观察它们特定角动量矢量的径向分布，我们发现固体模型不是一个合适的描述旋转运动的模型。暗物质速度的径向分布显示出普遍的随机速度色散。相反，集群内的介质配置文件的特点是从切向速度和色散的可比贡献。一般来说，暗物质成分主导了星系团的动力学，正如其角动量与气体角动量之间的相关性以及三组模拟之间缺乏相关差异所表明的那样。
英文摘要：
We present a study on the coherent rotation of the intracluster medium and dark matter components of simulated galaxy clusters extracted from a volume-limited sample of the MUSIC project. The set is re-simulated with three different recipes for the gas physics: $(i)$ non-radiative, $(ii)$ radiative without AGN feedback, and $(iii)$ radiative with AGN feedback. Our analysis is based on the 146 most massive clusters identified as relaxed, 57 per cent of the total sample. We classify these objects as rotating and non-rotating according to the gas spin parameter, a quantity that can be related to cluster observations. We find that 4 per cent of the relaxed sample is rotating according to our criterion. By looking at the radial profiles of their specific angular momentum vector, we find that the solid body model is not a suitable description of rotational motions. The radial profiles of the velocity of the dark matter show a prevalence of the random velocity dispersion. Instead, the intracluster medium profiles are characterized by a comparable contribution from the tangential velocity and the dispersion. In general, the dark matter component dominates the dynamics of the clusters, as suggested by the correlation between its angular momentum and the gas one, and by the lack of relevant differences among the three sets of simulations.
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