Thermodynamic perturbations in the X-ray halo of 33 clusters of galaxies observed with Chandra ACIS

TL;DR

This study analyzes high-resolution Chandra X-ray data of 33 galaxy clusters to measure thermodynamic perturbations in the intra-cluster medium, providing insights into turbulence and plasma properties relevant for future observatories.

Contribution

It presents the first large-sample analysis of thermodynamic perturbations in galaxy clusters using deep Chandra observations, constraining turbulence levels and correlations with metallicity.

Findings

Average Mach number of ICM turbulence ~ 0.16

Tight correlation between metallicity, temperature, and redshift

Provides detailed perturbation measurements for 33 clusters

Abstract

In high-resolution X-ray observations of the hot plasma in clusters of galaxies significant structures caused by AGN feedback, mergers, and turbulence can be detected. Many clusters have been observed by Chandra in great depth and at high resolution. Using archival data taken with the Chandra ACIS instrument the aim was to study thermodynamic perturbations of the X-ray emitting plasma and to apply this to better understand the thermodynamic and dynamic state of the intra cluster medium (ICM). We analysed deep observations for a sample of 33 clusters with more than 100 ks of Chandra exposure each at distances between redshift 0.025 and 0.45. The combined exposure of the sample is 8 Ms. Fitting emission models to different regions of the extended X-ray emission we searched for perturbations in density, temperature, pressure, and entropy of the hot plasma. For individual clusters we mapped the thermodynamic properties of the ICM and measured their spread in circular concentric annuli. Comparing the spread of different gas quantities to high-resolution 3D hydrodynamic simulations, we constrain the average Mach number regime of the sample to Mach1D ~ 0.16 +- 0.07. In addition we found a tight correlation between metallicity, temperature and redshift with an average metallicity of Z ~ 0.3 +- 0.1 Z(solar). This study provides detailed perturbation measurements for a large sample of clusters which can be used to study turbulence and make predictions for future X-ray observatories like eROSITA, Astro-H, and Athena.