An expanded merger-tree description of cluster evolution

Abstract

We model the formation and evolution of galaxy clusters in the framework of an extended dark matter halo merger-tree algorithm that includes baryons and incorporates basic physical considerations. Our modified treatment is employed to calculate the probability density functions of the halo concentration parameter, intracluster gas temperature, and the integrated Comptonization parameter for different cluster masses and observation redshifts. Scaling relations between cluster mass and these observables are deduced that are somewhat different than previous results. Modeling uncertainties in the predicted probability density functions are estimated. Our treatment and the insight gained from the results presented in this paper can simplify the comparison of theoretical predictions with results from ongoing and future cluster surveys.

11 pages, 9 figures, submitted to MNRAS

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Cited by in corpus (4)

• The Universal Einstein Radius Distribution from 10,000 SDSS Clusters
• Evolution of the gas mass fraction in galaxy clusters
• The effect of pressure-anisotropy-driven kinetic instabilities on magnetic field amplification in galaxy clusters
• SZ power spectrum and cluster numbers from an extended merger-tree model