Monte-Carlo Modeling of Non-Gravitational Heating Processes in Galaxy Clusters

Abstract

We consider non-gravitational heating effects on galaxy clusters on the basis of the Monte-Carlo modeling of merging trees of dark matter halos combined with the thermal evolution of gas inside each halo. Under the assumption of hydrostatic equilibrium and the isothermal gas profiles, our model takes account of the metallicity evolution, metallicity-dependent cooling of gas, supernova energy feedback, and heating due to jets of radio galaxies in a consistent manner. The observed properties of galaxy clusters can be explained in models with higher non-gravitational heating efficiency than that in the conventional model. Possibilities include jet heating by the Fanaroff-Riley Type II radio galaxies, and the enhanced star formation efficiency and/or supernova energy feedback, especially at high redshifts.

29 pages, 12 figures. To appear in PASJ, February 25, 2004

References in corpus (6)

• First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters
• The Birmingham-CfA cluster scaling project - III: entropy and similarity in galaxy systems
• Cooling and heating the ICM in hydrodynamical simulations
• The impact of galaxy formation on X-ray groups
• Mass-temperature relation of galaxy clusters: implications from the observed luminosity-temperature relation and X-ray temperature function
• Reliability of merger tree realizations of dark halos in the Monte-Carlo modeling of galaxy formation

Cited by in corpus (3)

• A Simple and Accurate Model for Intra-Cluster Gas
• Exploring the Energetics of Intracluster Gas with a Simple and Accurate Model
• Accurate Realizations of the Ionized Gas in Galaxy Clusters: Calibrating Feedback