Cluster correlation functions in N-body simulations
  The correlation function of galaxy clusters has often been used as a test of cosmological models. A number of assumptions are implicit in the comparison of theoretical expectations to data. Here we use an ensemble of ten large N-body simulations of the standard cold dark matter cosmology to investigate how cluster selection criteria and other uncertain factors influence the cluster correlation function. We consider the effects of varying the definition of a cluster, the mean number density (or equivalently the richness) in a catalogue, and the assumed normalisation of the model; we also examine the importance of redshift space distortions. We implement five different group-finding algorithms and construct cluster catalogues defined by mass, velocity dispersion or a measure of X-ray luminosity. We find that different cluster catalogues yield correlation functions which can differ by substantially more than the statistical errors in any one determination. For a given cluster selection criteria, the correlation length typically varies by $\sim 20\%$ in catalogues spanning the range of intercluster separations covered by the APM and Abell (richness class $\gsim 1$) catalogues. Distortions produced by peculiar velocities in redshift space enhance the correlation function at large separations and lead to a larger clustering length in redshift space than in real space. The sensitivity of the cluster correlation function to various uncertain model assumptions substantially weakens previous conclusions based on the comparison of model predictions with real data. Detailed modelling of cluster selection procedures including the effects of selecting from projected galaxy catalogues is required before the cluster correlation function can be regarded as a high precision constraint on cosmological models. 
Vincent R. Eke, Shaun Cole, Carlos S. Frenk (Durham) and Julio F.   Navarro (Steward Observatory, Univ. of Arizona)