On the impact of AGN feedback modes onto the turbulent properties of the multiphase ICM

TL;DR

This study uses hydrodynamic simulations to analyze how different AGN feedback modes influence turbulence in the intracluster medium, providing predictions for upcoming X-ray observations to better understand AGN energetics.

Contribution

It introduces detailed simulations of various AGN feedback modes and links their turbulent signatures to observable X-ray features, advancing understanding of AGN-ICM interactions.

Findings

Velocity dispersion correlates with AGN activity peaks.

Different feedback modes produce distinct turbulence profiles.

No significant kinematic coupling between hot and cold phases.

Abstract

The feedback from active galactic nuclei (AGN) plays a crucial role in regulating the thermodynamics and the dynamics of the intracluster medium (ICM). Studying the turbulent patterns of the hot and warm ionized phases may allow us to determine how these phases are involved in the AGN cycle and the amount of turbulent pressure generated by the latter. In this work, we use new simulations to study the turbulent motions created by different types of AGN feedback in a cool core cluster and predict the observable signatures with the latest X-ray telescopes (e.g. XRISM). We run several hydrodynamic simulations with ENZO, simulating the self-regulated cycles of AGN feedback, starting from a static ICM in a cluster that represents the Perseus cluster. We study in detail different feedback modes: from pure kinetic precessing jets up to almost pure thermal feedback. Our analysis reveals that the gas velocity dispersion in the center of the cluster correlates in time with the peaks of the AGN activity and that more than 50% of the time, different feedback modalities produce the velocity dispersion observed in the Perseus cluster while leading to distinct geometrical distributions and velocity dispersion profiles. Moreover, we do not find a significant kinematic coupling between the hot and the cold phase kinematics. We find a correlation between the AGN activity and the steepening of the velocity function structure (VSF) and that the projected 2D VSF slopes are never trivially correlated with the 3D VSF ones. This line of research will allow us to use incoming detections of gas turbulent motions detectable by XRISM (or future instruments) to better constrain the duty cycle, energetics and energy dissipation modalities of AGN feedback in massive clusters of galaxies.