The Three Hundred Project: The relationship between the shock and splashback radii of simulated galaxy clusters

作     者：Zhang, M. Walker, K. Sullivan, A. Power, C. Cui, W. Li, Y. Zhang, X. 

作者机构： College of Sciences Northeastern University Shenyang110819 China International Centre for Radio Astronomy Research The University of Western Australia 35 Stirling Highway CrawleyWA6009 Australia  Australia Departamento de Física Teórica Módulo 15 Facultad de Ciencias Universidad Autónoma de Madrid Madrid28049 Spain  Universidad Autónoma de Madrid Cantoblanco MadridE-28049 Spain Key Laboratory of Data Analytics and Optimization for Smart Industry Ministry of Education Northeastern University Shenyang110819 China National Frontiers Science Center for Industrial Intelligence and Systems Optimization Northeastern University Shenyang110819 China 

出 版 物：《arXiv》 (arXiv)

年 卷 期：2024年

核心收录：

主　　题：Dark Matter 

摘      要：Observations of the intracluster medium (ICM) in the outskirts of galaxy clusters reveal shocks associated with gas accretion from the cosmic web. Previous work based on non-radiative cosmological hydrodynamical simulations have defined the shock radius, rshock, using the ICM entropy, K ∝ T/ne2/3, where T and ne are the ICM temperature and electron density respectively;the rshock is identified with either the radius at which K is a maximum or at which its logarithmic slope is a minimum. We investigate the relationship between rshock, which is driven by gravitational hydrodynamics and shocks, and the splashback radius, rsplash, which is driven by the gravitational dynamics of cluster stars and dark matter and is measured from their mass profile. Using 324 clusters from The Three Hundred project of cosmological galaxy formation simulations, we quantify statistically how rshock relates to rsplash. Depending on our definition, we find that the median rshock 1.38rsplash(2.58R200) when K reaches its maximum and rshock 1.91rsplash(3.54R200) when its logarithmic slope is a minimum;the best-fit linear relation increases as rshock ∝ 0.65rsplash. We find that rshock/R200 and rsplash/R200 anti-correlate with virial mass, M200, and recent mass accretion history, and rshock/rsplash tends to be larger for clusters with higher recent accretion rates. We discuss prospects for measuring rshock observationally and how the relationship between rshock and rsplash can be used to improve constraints from radio, X-ray, and thermal Sunyaev-Zeldovich surveys that target the interface between the cosmic web and clusters. Copyright © 2024, The Authors. All rights reserved.