Abstract
I review observations and theoretical models of evolution of gas in clusters of galaxies. The mass of hot gas is an important component of clusters of galaxies, equalling or exceeding the total mass in galaxies in most clusters. The hot gas also traces the gravitational potential of the cluster, giving better measurements of the total mass of a cluster than those from velocity dispersions of the member galaxies. Clusters are still evolving, as expected from estimates of their dynamical times, and as observed in X-ray luminosity functions of clusters at different redshifts and in studies of subclustering. Theoretical models of how the intracluster gas might respond to a changing potential are important to interpretation of X-ray and optical data, particularly for clusters at high redshift. Models based on the standard assumptions of cold dark matter scenarios (and variations thereof) make predictions about cluster evolution. Finally I discuss the implications of the high ratios of gas to galaxy masses and of the iron abundances for the origin of the ICM.
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Donahue, M. (1993). Evolution of Clusters and the Intracluster Medium. In: Shull, J.M., Thronson, H.A. (eds) The Environment and Evolution of Galaxies. Astrophysics and Space Science Library, vol 188. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1882-8_23
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