Constraints on the total binding masses of three double clusters of galaxies

Details Constraints on the total binding masses of three double clusters of galaxies Constraints on the total binding masses of three double clusters of galaxies

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001phdt........13d&link_type=abstract

Thesis (PhD). DARTMOUTH COLLEGE, Source DAI-B 62/05, p. 2352, Nov 2001, 196 pages.

Computer Science

Scientific paper

The primary purpose of this research is to investigate the dynamics of pairs of galaxy clusters and the implications for cosmology. Substructure in galaxy clusters is common, indicating that many clusters are not yet virialized and that structure formation continues in the present epoch. When two clear subclusters can be identified, the radial infall model of Beers et al. (1982) (see also Peebles (1993)) can be applied to yield a mass estimate. The mass estimate may then be constrained sing the Fundamental Plane, a distance indicator for elliptical and lenticular galaxies. This work draws from the Abell (1958) catalog of clusters of galaxies. Three candidate pairs of clusters with components separated by less than 5 Mpc in projection and 1000 km/s in redshift were selected for study. In this thesis the radial infall model is applied to obtain a range of possible masses; Fundamental Plane distances are used to constrain those mass estimates; and the total binding masses of the clusters are compared to their virial masses. For two of the cluster pairs, significant discrepancies between the masses from radial infall and the virial masses are found. These may indicate errors or biases exist in the virial mass estimates; deviations from radial infall; or detection of mass outside the virial regions of the clusters. The N-body simulations of Navarro et al. (1997) produce a universal density profile shape, with more massive halos that are less centrally concentrated than less massive ones; this is consistent with detection of mass outside the virial regions of massive galaxy clusters. Additional spectroscopic data for the cluster pairs in this thesis is expected to better constrain their masses.

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