# Constraining Gas Motions in the Intra-Cluster Medium

## TL;DR

This paper reviews methods and recent measurements of gas velocities in the intra-cluster medium, highlighting their importance for understanding cluster physics and the microphysical properties of hot baryons.

## Contribution

It provides a comprehensive comparison of direct and indirect velocity measurement techniques and discusses their implications for cluster microphysics and turbulence sources.

## Key findings

- Recent Hitomi measurements of Perseus Cluster velocities.
- Comparison of multiple velocity estimation methods.
- Implications for ICM viscosity and turbulence sources.

## Abstract

The detailed velocity structure of the diffuse X-ray emitting intra-cluster medium (ICM) remains one of the last missing key ingredients in understanding the microphysical properties of these hot baryons and constraining our models of the growth and evolution of structure on the largest scales in the Universe. Direct measurements of the gas velocities from the widths and shifts of X-ray emission lines were recently provided for the central region of the Perseus Cluster of galaxies by $Hitomi$, and upcoming high-resolution X-ray microcalorimeters onboard $XRISM$ and $Athena$ are expected to extend these studies to many more systems. In the mean time, several other direct and indirect methods have been proposed for estimating the velocity structure in the ICM, ranging from resonant scattering to X-ray surface brightness fluctuation analysis, the kinematic Sunyaev-Zeldovich effect, or using optical line emitting nebulae in the brightest cluster galaxies as tracers of the motions of the ambient plasma. Here, we review and compare the existing estimates of the velocities of the hot baryons, as well as the various overlapping physical processes that drive motions in the ICM, and discuss the implications of these measurements for constraining the viscosity and identifying the source of turbulence in clusters of galaxies.