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Cosmological Simulations of Galaxy Clusters

机译：星系团的宇宙学模拟

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We review recent progress in the description of the formation and evolution of galaxy clusters in a cosmological context by using state-of-art numerical simulations. We focus our presentation on the comparison between simulated and observed X-ray properties, while we will also discuss numerical predictions on properties of the galaxy population in clusters, as observed in the optical band. Many of the salient observed properties of clusters, such as scaling relations between X-ray observables and total mass, radial profiles of entropy and density of the intracluster gas, and radial distribution of galaxies are reproduced quite well. In particular, the outer regions of cluster at radii beyond about 10 per cent of the virial radius are quite regular and exhibit scaling with mass remarkably close to that expected in the simplest case in which only the action of gravity determines the evolution of the intra-cluster gas. However, simulations generally fail at reproducing the observed "cool core" structure of clusters: simulated clusters generally exhibit a significant excess of gas cooling in their central regions, which causes both an overestimate of the star formation in the cluster centers and incorrect temperature and entropy profiles. The total baryon fraction in clusters is below the mean universal value, by an amount which depends on the cluster-centric distance and the physics included in the simulations, with interesting tensions between observed stellar and gas fractions in clusters and predictions of simulations. Besides their important implications for the cosmological application of clusters, these puzzles also point towards the important role played by additional physical processes, beyond those already included in the simulations. We review the role played by these processes, along with the difficulty for their implementation, and discuss the outlook for the future progress in numerical modeling of clusters.
机译：通过使用最新的数值模拟，我们回顾了在宇宙学背景下星系团的形成和演化描述中的最新进展。我们将介绍的重点放在模拟X射线和观察到的X射线属性之间的比较上，同时还将讨论对在光带中观察到的星团中星系种群的属性进行数值预测。很好地再现了星团的许多显着特性，例如X射线观测值与总质量之间的比例关系，熵的径向分布和团簇内气体的密度以及星系的径向分布。尤其是，半径超过病毒体半径约10％的簇的外部区域非常规则，并且在最简单的情况下只有质量的重力决定了内部星团的演化，其鳞片的质量显着接近预期。团簇气。但是，模拟通常无法重现观察到的星团的“冷核”结构：模拟星团通常在其中心区域显示出明显的气体冷却现象，这会导致高估星团中心的恒星形成以及不正确的温度和熵个人资料。团簇中的总重子分数低于平均通用值，该数量取决于团簇中心距离和模拟中包括的物理量，并且在团簇中观测到的恒星和气体分数之间以及与模拟预测之间存在有趣的张力。除了它们对星团的宇宙学应用的重要意义外，这些难题还指出了除了模拟中已经包含的物理过程之外，其他物理过程所起的重要作用。我们回顾了这些过程所扮演的角色，以及它们的实现难度，并讨论了集群数值建模的未来进展前景。

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