The intracluster medium (ICM) of galaxy clusters encodes the impact of the
physical processes that shape these massive halos, including feedback from
central supermassive black holes (SMBHs). In this study we examine the gas
thermodynamics, kinematics, and the effects of SMBH feedback on the core of
Perseus-like galaxy clusters with a new simulation suite: TNG-Cluster. We first
make a selection of simulated clusters similar to Perseus based on total mass
and inner ICM properties, i.e. cool-core nature. We identify 30 Perseus-like
systems among the 352 TNG-Cluster halos at z=0. Many exhibit thermodynamical
profiles and X-ray morphologies with disturbed features such as ripples,
bubbles and shock fronts that are qualitatively similar to X-ray observations
of Perseus. To study observable gas motions, we generate XRISM mock X-ray
observations and conduct a spectral analysis of the synthetic data. In
agreement with existing Hitomi measurements, TNG-Cluster predicts subsonic gas
turbulence in the central regions of Perseus-like clusters, with a typical
line-of-sight velocity dispersion of 200 km/s. This implies that turbulent
pressure contributes <10% to the dominant thermal pressure. In TNG-Cluster,
such low (inferred) values of ICM velocity dispersion coexist with
high-velocity outflows and bulk motions of relatively small amounts of
super-virial hot gas, moving up to thousands of km/s. However, detecting these
outflows observationally may prove challenging due to their anisotropic nature
and projection effects. Driven by SMBH feedback, such outflows are responsible
for many morphological disturbances in the X-ray maps of cluster cores. They
also increase both the inferred, and intrinsic, ICM velocity dispersion. This
effect is somewhat stronger when velocity dispersion is measured from
higher-energy lines.Comment: 14 pages, 8 figures. Submitted to A&A, comments welcome. See the
TNG-Cluster website at www.tng-project.org/cluster