The density and velocity fields as extracted from the Abell/ACO clusters are compared with 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 and 20 h(-1) Mpc. The density and velocity fields within 70 h(-1) Mpc 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 catalogues. Quantitative comparisons within a volume containing similar to 12 independent samples yield beta(c)=Omega(0.6)/b(c)=0.22 +/- 0.08, where b(c) is the cluster biasing parameter at 15 h(-1) Mpc. If b(c)similar to 4.5, as indicated by the cluster correlation function, our result is consistent with Omega similar to 1.

Branchini, E.F., Zehavi, I., Plionis, M., Dekel, A. (2000). Cluster versus POTENT density and velocity fields: cluster biasing and Omega. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 313(3), 491-503 [10.1046/j.1365-8711.2000.03257.x].

Cluster versus POTENT density and velocity fields: cluster biasing and Omega

BRANCHINI, ENZO FRANCO;
2000-01-01

Abstract

The density and velocity fields as extracted from the Abell/ACO clusters are compared with 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 and 20 h(-1) Mpc. The density and velocity fields within 70 h(-1) Mpc 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 catalogues. Quantitative comparisons within a volume containing similar to 12 independent samples yield beta(c)=Omega(0.6)/b(c)=0.22 +/- 0.08, where b(c) is the cluster biasing parameter at 15 h(-1) Mpc. If b(c)similar to 4.5, as indicated by the cluster correlation function, our result is consistent with Omega similar to 1.
Branchini, E.F., Zehavi, I., Plionis, M., Dekel, A. (2000). Cluster versus POTENT density and velocity fields: cluster biasing and Omega. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 313(3), 491-503 [10.1046/j.1365-8711.2000.03257.x].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11590/132232
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