Simulations of X-ray Clusters

We present simulations of the formation and evolution of galaxy clusters in the Cold Dark Matter cosmogony. Clusters with a wide range of mass were selected from previous N-body models, and were resimulated at higher resolution using a combined N-body/Smooth Particle Hydrodynamics code. The eeects of radiative cooling on the gas are neglected. While many present-day clusters are predicted to be undergoing mergers, the density prooles of those that are approximately in equilibrium are all very similar, both for the gas and for the dark matter. These prooles show no sign of a uniform density core and steepen gradually from the centre outwards. The standard-model is a reasonable t over most of the radius range observable in real clusters. However, the value obtained for the slope parameter f increases with the outermost radius of the t. Temperature prooles of diierent simulated clusters are also similar. Typically the temperature is almost uniform in the regions which emit most of the X-ray ux but drops at larger radii. The gas temperature and dark matter velocity dispersion in equilibrium clusters give values of T m p 2 DM =kT which are consistent with unity provided an X-ray emission-weighted temperature is used. Larger values of T are found in merging objects where there is a transient boost in the velocity dispersion of the system. Thus T > 1 may be an observational indicator of merging in real clusters. The similar structure of clusters of diiering mass results in scaling relations between the X-ray and dynamical properties of clusters identiied at any given redshift. These scalings are inconsistent with the observed slope of the luminosity-temperature relation or the observed sense of evolution of the cluster lumi-nosity function. This suggests that the central properties of the intracluster medium are determined by non-gravitational processes such as radiative cooling or substantial pre-heating at high redshift.