Measuring Ω_0 from the Entropy Evolution of Clusters

Abstract

In this paper, we have extended the entropy-driven model of cluster evolution developed by Bower (1997) in order to be able to predict the evolution of galaxy clusters for a range of cosmological scenarios. We have applied this model to recent measurements of the evolution of the L_x-T normalisation and X-ray luminosity function in order to place constraints on cosmological parameters. We find that these measurements alone do not select a particular cosmological frame-work. An additional constraint is required on the effective slope of the power spectrum to break the degeneracy that exists between this and the background cosmology. We have therefore included a theoretical calculation of the Ω_0 dependence on the power spectrum, based on the cold dark matter paradigm, which infers Ω_0<0.55 (0.1<Ω_0<0.7 for Ω_0+Λ_0=1), at the 95% confidence level. Alternatively, an independent measurement of the slope of the power spectrum from galaxy clustering requires Ω_0<0.6 (Ω_0<0.65 for Ω_0+Λ_0=1), again to 95% confidence. The rate of entropy evolution is insensitive to the values of Ω_0 considered, although is sensitive to changes in the distribution of the intracluster medium.

14 pages including 5 figures; accepted for publication in MNRAS

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• The WARPS survey - IV: The X-ray luminosity-temperature relation of high redshift galaxy clusters
• Temperature and Entropy Fields of Baryonic Gas in the Universe
• The Variation of Gas Mass Distribution in Galaxy Clusters: Effects of Preheating and Shocks
• The Effect of Formation Redshifts on the Cluster Mass-Temperature Relation
• A reanalysis of the luminosities of clusters of galaxies in the EMSS sample with 0.3 < z < 0.6
• Effects of Formation Epoch Distribution on X-Ray Luminosity and Temperature Functions of Galaxy Clusters