Going from galaxy clusters to galaxy groups: Cooling flows, AGN activity, and co-evolution of supermassive black holes with brightest halo galaxies

星系团和星系团与最亮的星系团/星系团星系（bcg /BGGs）的形成和演化以及位于这些星系中心的超大质量黑洞的共同演化有着复杂的联系。为了理解BCGs/BGGs和它们的宿主光晕以及超大质量黑洞之间固有的尺度关系，有必要揭示物理过程的影响，如气体冷却和AGN加热，对联系这些截然不同的结构特性的潜在参数的影响。在本提案中，我们首先简要描述了我们最近在该领域的贡献，该领域基于一个丰富的数据库，该数据库包括对统计上完整的星团尺度晕样本的射电和x射线观测，其次，我们提出了将该分析扩展到星团尺度的策略。嵌入在群尺度晕的较浅电位中心的AGN的反馈可能会更严重地影响周围气体的性质。我们的目标是将星团尺度和群体尺度的研究结果结合起来，以获得对星系和超大质量黑洞的演化以及星团内气体的冷却和加热的更连贯和完整的理解。

Galaxy clusters and groups are intricately tied to the formation and evolution of brightest cluster / group galaxies (BCGs/BGGs), and the co-evolution of supermassive black holes residing at centers of these galaxies. To understand the inherent scaling relations between BCGs/BGGs and both, their host halos as well as supermassive black holes, it is imperative to unravel the effects of physical processes, such as gas cooling and AGN heating, on the underlying parameters that tie the properties of these vastly different regimes of structures. In this proposal, we first briefly describe our recent contributions to this field based on a rich database comprising radio and X-ray observations of a statistically complete sample of cluster-scale halos and second, our proposed strategy to extend this analysis to the group scale. Feedback from an AGN embedded at the center of a shallower potential of a group-scale halo is likely to more severely affect the properties of the surrounding gas. Our aim is to combine results from the cluster-scale and group-scale studies to gain a more coherent and complete understanding of the evolution of galaxies and supermassive black holes, along with the cooling and heating of the intracluster gas.