Baryon fractions in clusters of galaxies: evidence against a preheating model for entropy generation

TL;DR

This study compares galaxy cluster simulations with observations, finding that models with early preheating do not match observed hot gas fractions, suggesting continual feedback models are more accurate.

Contribution

It provides a comparative analysis of different physical heating mechanisms in galaxy cluster simulations against observational data.

Findings

Simulations match hot gas profiles of non-cool-core clusters.

Early preheating models show larger evolution in hot gas fraction than observed.

Simulations poorly reproduce stellar fractions and their dependence on cluster mass.

Abstract

The Millennium Gas project aims to undertake smoothed-particle hydrodynamic resimulations of the Millennium Simulation, providing many hundred massive galaxy clusters for comparison with X-ray surveys (170 clusters with kTsl > 3 keV). This paper looks at the hot gas and stellar fractions of clusters in simulations with different physical heating mechanisms. These fail to reproduce cool-core systems but are successful in matching the hot gas profiles of non-cool-core clusters. Although there is immense scatter in the observational data, the simulated clusters broadly match the integrated gas fractions within r500 . In line with previous work, however, they fare much less well when compared to the stellar fractions, having a dependence on cluster mass that is much weaker than is observed. The evolution with redshift of the hot gas fraction is much larger in the simulation with early preheating than in one with continual feedback; observations favour the latter model. The strong dependence of hot gas fraction on cluster physics limits its use as a probe of cosmological parameters.