Cluster versus POTENT Density and Velocity Fields: Cluster Biasing and Omega

Abstract

The density and velocity fields as extracted from the Abell/ACO clusters are compared to the corresponding fields recovered by the POTENT method from the Mark~III peculiar velocities of galaxies. In order to minimize non-linear effects and to deal with ill-sampled regions we smooth both fields using a Gaussian window with radii ranging between $12 - 20\hmpc$. The density and velocity fields within $70\hmpc$ exhibit similarities, qualitatively consistent with gravitational instability theory and a linear biasing relation between clusters and mass. The random and systematic errors are evaluated with the help of mock catalogs. Quantitative comparisons within a volume containing $\sim 12$ independent samples yield $\betac\equivΩ^{0.6}/b_c=0.22\pm0.08$, where $b_c$ is the cluster biasing parameter at $15\hmpc$. If $b_c\sim 4.5$, as indicated by the cluster correlation function, our result is consistent with $\Omega \sim 1$.

18 pages, latex, 2 ps figures 6 gif figures. Accepted for pubblications in MNRAS

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