The Evolution and Mass Dependence of Galaxy Cluster Pressure Profiles at 0.05 ≤ z ≤ 0.60 and 4 × 10¹⁴ M _⊙ ≤ M ₅₀₀ ≤ 30 × 10¹⁴ M _⊙

Abstract

We have combined X-ray observations from Chandra with Sunyaev–Zel’dovich effect data from Planck and Bolocam to measure intracluster medium pressure profiles from 0.03 R 500 ≤ R ≤ 5 R 500 for a sample of 21 low-z galaxy clusters with a median redshift of 〈z〉 = 0.08 and a median mass of 〈M 500〉 = 6.1 × 1014 M ⊙ and a sample of 19 mid-z galaxy clusters with 〈z〉 = 0.50 and 〈M 500〉 = 10.6 × 1014 M ⊙. 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 The Three Hundred 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 the mass accretion rate and the fractional impact of feedback mechanisms. In agreement with previous studies, the fractional scatter about the mean scaled pressure profile reaches a minimum of ≃20% near 0.5 R 500. This scatter is consistent between the low-z and mid-z samples at all radii, suggesting it is not strongly impacted by sample selection, and this general behavior is reproduced in The Three Hundred simulations. Finally, analytic functions that approximately describe the mass and redshift trends in mean pressure profile shape are provided.

Joint measurement of the galaxy cluster pressure profile with Planck and SPT-SZ

“…Similarly Pointecouteau et al (2021) used the Planck and ACT data jointly to measure the average pressure profile of 31 clusters, demonstrating that space-based and ground-based data can be efficiently combined to improve constraints on the cluster pressure profile. Finally, Sayers et al (2023) combined Bolocam, Planck and Chandra data to study the redshift evolution and mass dependence of the average pressure profile of 40 clusters.…”

Shocks in the stacked Sunyaev-Zel’dovich profiles of clusters II: Measurements from SPT-SZ + Planck Compton-y map

“…The first studies used nonradiative simulations with gas dynamics but no astrophysical processes (Quilis et al 1998;Miniati et al 2000;Ryu et al 2003;Skillman et al 2008;Molnar et al 2009;Hong et al 2014Hong et al , 2015Schaal & Springel 2015). These were then followed by studies using simulations that include gas cooling and star formation (Vazza et al 2009;Planelles & Quilis 2013;Lau et al 2015;Nelson et al 2016;Aung et al 2021), and also include the effects of feedback from supernovae and active galactic nuclei (Kang et al 2007;Vazza et al 2013Vazza et al , 2014Schaal et al 2016;Baxter et al 2021;Planelles et al 2021;Baxter et al 2023;Sayers et al 2023). Some works have also opted to model the evolution of cosmic-rays -which are generated at the shocks -alongside galaxy formation (Pfrommer et al 2007), while others employ idealized simulations to understand the propagation of shocks and their dependence on different merger events (Pfrommer et al 2006;Ha et al 2018;Zhang et al 2019bZhang et al , 2020Zhang et al , 2021.…”