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D. Gudehus (Georgia State University)
N-body simulations of gravitationally induced peculiar motions from a set of 1009 clusters of known redshift give reasonably good agreement for the peculiar velocities of the Local Group and Virgo both in magnitude and direction. Using physically realistic values for the ten adjustable parameters in the model, I find that the best correspondence with observation occurs when an amount of mass greater than that given by the cluster velocity dispersion, and increasing with cluster richness, is assigned to the clusters. In other words, increasing amounts of mass located outside the richer clusters, but associated with them, are required to reproduce the peculiar velocities. Most of the accelerating mass of the cluster set lies within about 40h-1 Mpc of the Local Group, but more distant clusters are necessary to fully account for the magnitude and direction of the peculiar velocities.
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