Clustering of galaxy clusters in CDM universes

We use very large cosmological N–body simulations to obtain accurate predictions for the two-point correlations and power spectra of mass-limited samples of galaxy clusters. We consider two currently popular cold dark matter (CDM) cosmogonies, a critical density model (�CDM) and a flat low density model with a cosmological constant (�CDM). Our simulations each use 10 9 particles to follow the mass distribution within cubes of side 2h 1 Gpc (�CDM) and 3h 1 Gpc (�CDM) with a force resolution better than 10 4 of the cube side. We investigate how the predicted cluster correlations increase for samples of increasing mass and decreasing abundance. Very similar behaviour is found in the two cases. The correlation length increases from r0 = 12 – 13h 1 Mpc for samples with mean separation dc = 30h 1 Mpc to r0 = 22 – 27h 1 Mpc

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