SZ power spectrum and cluster numbers from an extended merger-tree model

Abstract

We have recently developed an extended merger-tree model that efficiently follows hierarchical evolution of galaxy clusters and provides a quantitative description of both their dark matter and gas properties. We employed this diagnostic tool to calculate the thermal SZ power spectrum and cluster number counts, accounting explicitly for uncertainties in the relevant statistical and intrinsic cluster properties, such as the halo mass function and the gas equation of state. Results of these calculations are compared with those obtained from a direct analytic treatment and from hydrodynamical simulations. We show that under certain assumptions on the gas mass fraction our results are consistent with the latest SPT measurement. Our approach can be particularly useful in predicting cluster number counts and their dependence on cluster and cosmological parameters.

8 pages, 7 figures, accepted for publication in MNRAS

References in corpus (11)

• The redshift dependence of the structure of massive LCDM halos
• Stellar and total baryon mass fractions in groups and clusters since redshift 1
• Generating Dark Matter Halo Merger Trees
• Calibration of the galaxy cluster M_500-Y_X relation with XMM-Newton
• The dark matter halos of massive, relaxed galaxy clusters observed with Chandra
• The Observed Concentration-Mass Relation for Galaxy Clusters
• The Effect of Gas Physics on the Halo Mass Function
• Sharpening the Precision of the Sunyaev-Zel'dovich Power Spectrum
• The Sunyaev-Zel'dovich effects from a cosmological hydrodynamical simulation: large-scale properties and correlation with the soft X-ray signal
• Cluster abundances and S-Z power spectra: effects of non-Gaussianity and early dark energy
• The Sunyaev-Zeldovich Background

Cited by in corpus (2)

• Evolution of the gas mass fraction in galaxy clusters
• Constraints on the Neutrino Mass from SZ Surveys