Interactions between Active Galactic Nuclei and the Intracluster Medium

活动星系核(AGN)和星系团内介质(ICM)之间的相互作用对于反馈是必不可少的，后者被认为是星系形成的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描述了M87、九头蛇A和M84中的活动星系核-ICM相互作用，我们发现湍流是塑造气泡演化的原因，我们正在将AGN反馈纳入宇宙学模拟。在下一阶段，我们希望解决AGN和ICM之间相互作用的一些尚不清楚的方面。我们希望追溯活动星系核的历史，这段历史导致了明亮的星系团M87和九头蛇A的复杂结构，我们对这些星团进行了新的、深入的观测。在这里，我们重点介绍我们将在流体力学模拟中再现的叶结构和冷锋。此外，我们希望限制X射线腔的性质，并验证目前估计驻留在腔中的能量的方法。这与我们在宇宙学模拟中包含的活动星系核反馈的性质密切相关。他们将给出冷核心的统计数据的预测，我们将用统计选择的各种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.