The Inner Slope of the Mass Density in Groups and Clusters of Galaxies

Details The Inner Slope of the Mass Density in Groups and Clusters of Galaxies The Inner Slope of the Mass Density in Groups and Clusters of Galaxies

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19914204m&link_type=abstract

American Astronomical Society, 199th AAS Meeting, #142.04; Bulletin of the American Astronomical Society, Vol. 33, p.1521

Mathematics

Probability

Scientific paper

We improve existing techniques for constraining the mass profile and orbital structure of nearby groups and clusters of galaxies. Our method yields the joint probability distribution of the inner density slope λ , the velocity anisotropy, and the core radius for these systems. We incorporate 2419 new redshifts in the fields of 41 groups of galaxies with z < 0.04, as well as 1181 archived redshifts in the fields of 10 dynamically relaxed clusters with z < 0.1. We combine groups and clusters that have statistically consistent velocity dispersion profiles (VDPs); these turn out to be systems with declining VDPs, even though we place no requirements on the VDP shapes when we test for consistency. Our analysis yields λ = 1.3-1.9 for groups and λ = 0-0.7 for clusters, suggesting that richer systems of galaxies have flatter dark matter density profiles.

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