Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.4501b&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #45.01; Bulletin of the American Astronomical Society, Vol. 24, p.1191
Other
Scientific paper
The evolution of clusters of galaxies is investigated with the use of self-consistent N-body simulations. Previous simulations have either used a Fokker-Planck treatment of the evolution of the galaxy distribution or have followed the trajectories of individual galaxies; in neither case has their internal structure been resolved. A unified treatment which directly simulates the evolution of a cluster of realistic, extended galaxies is clearly preferable. Five full N-body simulations, with each galaxy represented as an extended structure, have been carried out using N=4*E(4) particles. Half of the particles are in a cluster `dark matter' background; the other half are in galaxies. There are initially fifty galaxies with a Schechter function mass distribution. The galaxies themselves are King models, with the most bound particles identified as belonging to a `luminous' core such that the luminous fraction is 10%. The clusters are initially in a virialized state (a W0=6 King model) and their evolution is followed for roughly a Hubble time, using a direct N-body `tree' code employing a modified version of Hernquist's implementation of the Barnes-Hut tree algorithm. The five runs differ in that the galaxies are given different random initial positions and velocities; the merging history varies little between the runs. All five show the growth of a dominant, centrally located galaxy due to succesive mergers; the lower-mass galaxies are much less affected by merging. We will present results on the evolution of the mass function and spatial distribution of the galaxies. The effect of increasing the cluster background mass fraction will also be examined.
Bode Paul W.
Cohn Haldan N.
Lugger Phyllis Minnie
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