Open AccessCan simulations reproduce the observed temperature–mass relation for clusters of galaxies?
Author(s) -
Thomas Peter A.,
Muanwong Orrarujee,
Kay Scott T.,
Liddle Andrew R.
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05307.x
Subject(s) - physics , astrophysics , galaxy cluster , normalization (sociology) , cluster (spacecraft) , galaxy , radiative cooling , galaxy groups and clusters , brightest cluster galaxy , galaxy formation and evolution , perturbation (astronomy) , radiative transfer , astronomy , quantum mechanics , sociology , anthropology , computer science , programming language
It has become increasingly apparent that traditional hydrodynamical simulations of galaxy clusters are unable to reproduce the observed properties of galaxy clusters, in particular overpredicting the mass corresponding to a given cluster temperature. Such overestimation may lead to systematic errors in results using galaxy clusters as cosmological probes, such as constraints on the density perturbation normalization σ 8 . In this paper we demonstrate that inclusion of additional gas physics, namely radiative cooling and a possible pre‐heating of gas prior to cluster formation, is able to bring the temperature–mass relation in the innermost parts of clusters into good agreement with recent determinations by Allen, Schmidt & Fabian using Chandra data.