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The Evolution and Mass Dependence of Galaxy Cluster Pressure Profiles at 0.05 $\le z \le$ 0.60 and $4 \times 10^{14}$ M$ {\odot}$ $\le \textrm{M} {500} \le 30 \times 10^{14}$ M$ {\odot}$ by Sayers, Jack; Mantz, Adam B.; Rasia, Elena; Allen, Steven W.; Cui, Weiguang; Golwala, Sunil R.; Morris, R. Glenn; Wan, Jenny T. is a scholarly article available to read on EtoBox.

What is The Evolution and Mass Dependence of Galaxy Cluster Pressure Profiles at 0.05 $\le z \le$ 0.60 and $4 \times 10^{14}$ M$ {\odot}$ $\le \textrm{M} {500} \le 30 \times 10^{14}$ M$ {\odot}$ about?

We have combined X-ray observations from Chandra with Sunyaev-Zel'dovich (SZ) effect data from Planck and Bolocam to measure intra-cluster medium pressure profiles from 0.03R$_{500}$ $\le$ R $\le$ 5R$_{500}$ for a sample of 21 low-$z$ galaxy clusters with a median redshift $\langle z \rangle = 0.08$ and a median mass $\langle \textrm{M}_{500} \rangle = 6.1 \times 10^{14}$ M$_{\odot}$ and a sample of 19 mid-$z$ galaxy clusters with $\langle z \rangle = 0.50$ and $\langle \textrm{M}_{500} \rangle = 10.6 \times 10^{14}$ M$_{\odot}$. The mean scaled pressure in the low-$z$ sample is lower at small radii and higher at large radii, a trend that is accurately reproduced in similarly selected samples from The300 simulations. This difference appears to be primarily due to dynamical state at small radii, evolution at intermediate radii, and a combination of evolution and mass dependence at large radii. Furthermore, the overall flattening of the mean scaled pressure profile in the low-$z$ sample compared to the mid-$z$ sample is consistent with expectations due to differences in mass accretion rate and the fractional impact of feedback mechanisms. In agreement with previous studies, the fract

Author

Sayers, Jack; Mantz, Adam B.; Rasia, Elena; Allen, Steven W.; Cui, Weiguang; Golwala, Sunil R.; Morris, R. Glenn; Wan, Jenny T.

Published

2022

Language

EN