Observations and amr Simulations of the Evolution of Galaxy Clusters

We will present preliminary results from a numerical survey of galaxy groups and clusters using a new high spatial dynamic range, Eulerian, adapative mesh refinement, N-body/hydro code. The simulations were performed for an {Omega_o} + {Omega_lambda} = 1 CDM Universe. We will discuss the evolution of the cluster mass, X-ray, and temperature functions, and will present initial results on the evolution of X-ray and temperature substructure, bulk flows, merger histories, and cooling flows. These numerical results will be compared with new ROSAT HRI, optical, and radio observations of z >= 0.2 Abell clusters and nearby poor clusters.