Simulations of AGN Feedback in Galaxy Clusters and Groups: Impact on Gas Fractions and the LX-T Scaling Relation
Simulations of AGN Feedback in Galaxy Clusters and Groups: Impact on Gas Fractions and the LX-T Scaling Relation
复制标题
星系团和星系群中 AGN 反馈的模拟：对气体分数和 LX-T 尺度关系的影响
DOI：
10.1086/593352
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发表时间：
2008
期刊：
影响因子：
--
通讯作者：
V. Springel
中科院分区：
文献类型：
--
作者：
E. Puchwein;D. Sijacki;V. Springel
近年来，随着观测和理论的快速发展，黑洞在单个星系以及星系群和星系团的形成和演化中起着决定性的作用。特别是，有令人信服的证据表明，黑洞在星系团的中心区域与周围环境发生了强烈的相互作用，这表明任何现实的星系团形成模型都需要考虑这些过程。前几代没有BH物理的流体动力学模拟的失败也表明了这一点，这些模拟同时解释了星系团中强冷却流的缺乏、观测到的星系团标度关系的斜率和振幅以及星系团中央星系的高光度截止。在这里，我们使用高分辨率的宇宙学模拟的一个大的集群和组的样本，研究黑洞如何影响他们的主机系统。我们专注于两个特定的属性，晕气体分数和X射线的亮度-温度的标度关系，这两者都是出了名的难以重现自洽流体动力学模拟。我们表明，BH反馈可以解决这两个问题，使它们与观测结果非常一致，而不是暗指产生非物理明亮的中央星系的“仅冷却”解决方案。通过将模拟活动星系核加热的星团的大样本与观测结果进行比较，我们的新模拟技术应该能够可靠地校准星团调查中的观测偏差，从而实现对宇宙暗物质和暗能量含量的各种高精度宇宙学研究。
Recently, rapid observational and theoretical progress has established that black holes (BHs) play a decisive role in the formation and evolution of individual galaxies as well as galaxy groups and clusters. In particular, there is compelling evidence that BHs vigorously interact with their surroundings in the central regions of galaxy clusters, indicating that any realistic model of cluster formation needs to account for these processes. This is also suggested by the failure of previous generations of hydrodynamical simulations without BH physics to simultaneously account for the paucity of strong cooling flows in clusters, the slope and amplitude of the observed cluster scaling relations, and the high-luminosity cutoff of central cluster galaxies. Here we use high-resolution cosmological simulations of a large cluster and group sample to study how BHs affect their host systems. We focus on two specific properties, the halo gas fraction and the X-ray luminosity-temperature scaling relation, both of which are notoriously difficult to reproduce in self-consistent hydrodynamical simulations. We show that BH feedback can solve both of these issues, bringing them in excellent agreement with observations, without alluding to the “cooling only” solution that produces unphysically bright central galaxies. By comparing a large sample of simulated AGN-heated clusters with observations, our new simulation technique should make it possible to reliably calibrate observational biases in cluster surveys, thereby enabling various high-precision cosmological studies of the dark matter and dark energy content of the universe.