巨大而精致：高分辨率模拟的大型星系团样本。一：热气和shock waves性质
Massive and refined: a sample of large galaxy clusters simulated at high resolution. I:Thermal gas and shock waves properties
摘要：
我们提出了一个样本的20个大质量的星系团的维里质量的范围为6 10^14 M_sol<M（vir）< 2 10^15 M_sol，重新模拟与定制版本的1.5。ENZO代码采用自适应网格细化。这种技术使我们能够获得前所未有的高空间分辨率（25 kpc/h），距离3维里半径的集群中心，并使其能够专注于相同水平的细节上的最内层和最外层的集群区域的物理特性，提供新的线索的冲击波和湍流运动的作用在ICM中，在广泛的尺度。在本文中，这个数据集的第一个探索性研究。我们报道了z=0时星系团的热性质。综合和形态性质的气体密度，气体温度，气体熵和重子分数分布进行了讨论，并与现有的结果都从观测和数值文献进行了比较。我们的集群样本显示出整体良好的一致性，采用其他数值技术（例如光滑粒子流体力学）获得的结果，但它提供了一个更准确的表示吸积模式远离集群核心。我们还重建的样品内的冲击波的性质，通过一个基于速度的方法，我们研究的马赫数和能量分布的各种动力学状态的集群，估计注入的宇宙射线粒子在冲击。本样本是相当独特的全景宇宙学模拟的大规模星系团，由于其动态范围，统计对象和时间输出的数量。出于这个原因，我们部署了一个可用数据的公共存储库，可以通过门户网站http://data.cineca.it访问。
英文摘要：
We present a sample of 20 massive galaxy clusters with total virial masses in the range of 6 10^14 M_sol<M(vir)< 2 10^15M_sol, re-simulated with a customized version of the 1.5. ENZO code employing Adaptive Mesh Refinement. This technique allowed us to obtain unprecedented high spatial resolution (25kpc/h) up to the distance of 3 virial radii from the clusters center, and makes it possible to focus with the same level of detail on the physical properties of the innermost and of the outermost cluster regions, providing new clues on the role of shock waves and turbulent motions in the ICM, across a wide range of scales. In this paper, a first exploratory study of this data set is presented. We report on the thermal properties of galaxy clusters at z=0. Integrated and morphological properties of gas density, gas temperature, gas entropy and baryon fraction distributions are discussed, and compared with existing outcomes both from the observational and from the numerical literature. Our cluster sample shows an overall good consistency with the results obtained adopting other numerical techniques (e.g. Smoothed Particles Hydrodynamics), yet it provides a more accurate representation of the accretion patterns far outside the cluster cores. We also reconstruct the properties of shock waves within the sample by means of a velocity-based approach, and we study Mach numbers and energy distributions for the various dynamical states in clusters, giving estimates for the injection of Cosmic Rays particles at shocks. The present sample is rather unique in the panorama of cosmological simulations of massive galaxy clusters, due to its dynamical range, statistics of objects and number of time outputs. For this reason, we deploy a public repository of the available data, accessible via web portal at http://data.cineca.it.
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