Evolution of the gas mass fraction in galaxy clusters

Abstract

The mass fraction of hot gas in clusters is a basic quantity whose level and dependence on the cluster mass and redshift are intimately linked to all cluster X-ray and SZ measures. Modeling the evolution of the gas fraction is clearly a necessary ingredient in the description of the hierarchical growth of clusters through mergers of subclumps and mass accretion on the one hand, and the dispersal of gas from the cluster galaxies by tidal interactions, galactic winds, and ram pressure stripping on the other hand. A reasonably complete description of this evolution can only be given by very detailed hydrodynamical simulations, which are, however, resource-intensive, and difficult to implement in the mapping of parameter space. A much more practical approach is the use of semi-analytic modeling that can be easily implemented to explore a wide range of parameters. We present first results from a simple model that describes the build up of the gas mass fraction in clusters by following the overall impact of the above processes during the merger and accretion history of each cluster in the ensemble. Acceptable ranges for model parameters are deduced through comparison with results of X-ray observations. Basic implications of our work for modeling cluster statistical properties, and the use of these properties in joint cosmological data analyses, are discussed.

10 pages, 6 figures, updated to match MNRAS accepted version

References in corpus (17)

• Heating Hot Atmospheres with Active Galactic Nuclei
• Chandra temperature profiles for a sample of nearby relaxed galaxy clusters
• Stellar and total baryon mass fractions in groups and clusters since redshift 1
• Generating Dark Matter Halo Merger Trees
• LoCuSS: Comparison of Observed X-ray and Lensing Galaxy Cluster Scaling Relations with Simulations
• X-ray cavities in a sample of 83 SPT-selected clusters of galaxies: Tracing the evolution of AGN feedback in clusters of galaxies out to z=1.2
• The Redshift Evolution of the Mean Temperature, Pressure, and Entropy Profiles in 80 SPT-Selected Galaxy Clusters
• The extended ROSAT-ESO Flux Limited X-ray Galaxy Cluster Survey (REFLEX II) IV. X-ray Luminosity Function and First Constraints on Cosmological Parameters
• Exploring the Energetics of Intracluster Gas with a Simple and Accurate Model
• Ram pressure stripping in a galaxy formation model. I. A novel numerical approach
• Revisiting the Baryon Fractions of Galaxy Clusters: A Comparison with WMAP 3-year Results
• Probing the truncation of galaxy dark matter halos in high density environments from hydrodynamical N-body simulations
• Metal enrichment of the intra-cluster medium over a Hubble time for merging and relaxed galaxy clusters
• Ram pressure histories of cluster galaxies
• Cosmological Simulations of the Preheating Scenario for Galaxy Cluster Formation: Comparison to Analytic Models and Observations
• The Most Massive Black Holes in the Universe: Effects of Mergers in Massive Galaxy Clusters
• The Origin of Dark Matter Halo Profiles

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