The redshift-space power spectrum of Abell-ACO clusters of galaxies

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  • 5 September 1997
Abstract
We use a redshift sample of Abell-ACO R>=0 clusters with 401 measured and 16 estimated redshifts to derive the 2-point correlation function and the power spectrum of their redshift-space distribution. We find that the average value of the 2-point function within a sphere of radius R=30 Mpc/h is <\xi(R)> = 0.85+-0.15. Over the scale range 10 <= R <= 40 Mpc/h, the power law <\xi(R)> \propto R^{-1.8} is a good approximation. The power spectrum is reliably estimated for 0.03 <= k <= 0.2 h/Mpc. For k>k_{max} \simeq 0.05 h/Mpc it has a power law shape, P(k) \propto k^n, with n \approx -1.9, while it changes sharply to a positive slope at k < k_{max}. The power spectrum of clusters lies above that of galaxies, thus suggesting b \sim 3 for the relative galaxy-cluster biasing parameter. A comparision with mock catalogues from large PM simulations for four cosmological models rejects standard CDM and tilted CDM (n_{pr}=0.9). It shows some better agreement with a \LambdaCDM model with \Omega_0=0.35 and h=0.7 and with a CDM model with broken scale invariance (BSI). However, in no cases we find that simulations produce a P(k) slope for k > k_{max} as steep as that found for Abell-ACO clusters.

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