Interactions between Active Galactic Nuclei and the Intracluster Medium

活动星系核（AGN）和团内介质（ICM）之间的相互作用是反馈的必要条件，而反馈被认为是星系形成重子部分的关键成分。我们申请继续我们的项目，在这个项目中，我们在理解活动星系核反馈的物理学方面取得了实质性进展：我们通过观测和流体动力学模拟的协调方法，我们发现湍流是形成气泡演化的原因，我们正在宇宙学模拟中加入活动星系核反馈。在下一阶段，我们希望解决活动星系核和ICM之间的相互作用的一些方面仍然不清楚。我们希望追溯活动星系核的历史，这导致了明亮的星团M87和Hydra A的复杂结构，我们对它们进行了新的深层观测。在这里，我们专注于瓣结构和冷锋，我们将重现在流体动力学模拟。此外，我们希望约束的性质的X射线腔和验证目前的方法估计驻留在腔中的能量。这与我们在宇宙学模拟中所包含的活动星系核反馈的性质密切相关。他们将给出冷核统计的预测，我们将用统计选择的不同红移的星团样本进行测试。

The interaction between active galactic nuclei (AGN) and the intracluster medium (ICM) is essential for feedback, which is believed to be the crucial ingredient for the baryonic part of galaxy formation. We apply for a continuation of our project in which we made substantial progress in understanding the physics of AGN feedback: We characterised the AGN-ICM interactions in M87, Hydra A and M84 by a concerted approach of observations and hydrodynamic simulations, we found that turbulence is responsible for shaping the evolution of the bubbles and we are incorporating AGN feedback in cosmological simulations.In the next phase we wish to address some aspects of the interaction between AGN and ICM that remain unclear. We wish to retrace the AGN history that has led to the complex structure of the bright clusters M87 and Hydra A for which we have new, deep observations. Here, we focus on the lobe structures and cold fronts that we will reproduce in hydrodynamical simulations. Moreover, we wish to constrain the nature of X-ray cavities and validate current methods of estimating the energies residing in cavities. This is closely related to the nature of AGN feedback that we are including in cosmological simulations. They will give predictions for the statistics of cool cores which we will test with statistically selected samples of clusters at various redshifts.