星系团图中相关和散射的流体动力学模拟
Hydrodynamic simulations of correlation and scatter in galaxy cluster maps
摘要：
星系团中热气体的二维结构包含着星系团流体动力学状态的信息，它可以用来理解气体热力学性质散射的起源，并有助于星系团在宇宙学研究中的应用。使用一组流体动力学模拟，我们提供了目前采用的各种地图之间的比较合并集群的X射线分析和那些集群地图预计从即将到来的观测热Sunyaev-Zel 'dovich效应。我们显示以下内容：1）X射线伪压力，定义为软带X射线图像乘以温度图的平方根，是SZ图的良好代理; 2）我们发现，团块是X射线伪压力和SZ图之间偏差的主要原因; 3）团块的水平可以很好地由X射线伪熵图表征。4)我们描述的频率的偏差在各种地图的集群作为偏差的幅度的函数。这使得既可以与观察结果进行比较，也可以与将复杂物理过程引入模拟的效果进行比较。
英文摘要：
The two dimensional structure of hot gas in galaxy clusters contains information about the hydrodynamical state of the cluster, which can be used to understand the origin of scatter in the thermodynamical properties of the gas, and to improve the use of clusters to probe cosmology. Using a set of hydrodynamical simulations, we provide a comparison between various maps currently employed in the X-ray analysis of merging clusters and those cluster maps anticipated from forthcoming observations of the thermal Sunyaev-Zel'dovich effect. We show the following: 1) an X-ray pseudo-pressure, defined as square root of the soft band X-ray image times the temperature map is a good proxy for the SZ map; 2) we find that clumpiness is the main reason for deviation between X-ray pseudo-pressure and SZ maps; 3) the level of clumpiness can be well characterized by X-ray pseudo-entropy maps. 4) We describe the frequency of deviation in various maps of clusters as a function of the amplitude of the deviation. This enables both a comparison to observations and a comparison to effects of introduction of complex physical processes into simulation.
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