Abstract
The character of the galaxy cluster population holds clues to the identity of the particular world model that best describes our universe. Although clusters are complex in their fine detail, their dark matter and intracluster medium (ICM) content appear to be well described by relatively simple processes driven by gravitationally induced mergers. After reviewing theoretical frameworks of spherical collapse and hierarchical clustering, we separate the problem of extracting cosmological parameters from observations into two parts: describing the space density of clusters as a function of total mass and calibrating relations that connect total mass to observable quantities.
Guided by computational modeling of cluster formation, we examine the effects of cluster mergers on their hydrostatic boundaries, on their internal density structure, and on the variance exhibited about the mean virial relation connecting mass to temperature. We summarize constraints on the clustered matter density ωm and power spectrum normalization σ8 derived from X-ray observations of the ICM, including new estimates of systematic uncertainties in these measures derived from Hubble Volume simulations. The mean baryon fraction of clusters presents the most precise contraint favoring a low density universe, ω m (h/0.7)2/3=0.30±(0.02)stat±(0.06)sys with uncertainty in the mass-temperature relation being the leading source of systematic error.
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Evrard, A.E., Gioia, I.M. (2002). Clusters, Cosmology and Mergers. In: Feretti, L., Gioia, I.M., Giovannini, G. (eds) Merging Processes in Galaxy Clusters. Astrophysics and Space Science Library, vol 272. Springer, Dordrecht. https://doi.org/10.1007/0-306-48096-4_9
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