Simulation of compact groups of galaxies

Details Simulation of compact groups of galaxies Simulation of compact groups of galaxies

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.119..221i&link_type=abstract

(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),

Statistics

Computation

14

Computerized Simulation, Galactic Clusters, Missing Mass (Astrophysics), Spiral Galaxies, Computational Astrophysics, Galactic Evolution, Galactic Structure, Gravitational Collapse, Halos, Hubble Constant, Radii, Velocity Distribution, Virial Theorem

Scientific paper

Self-consistent simulations of seven groups of galaxies with halos have been performed to find a constraint upon the size of missing halos around spiral galaxies. An initial galaxy, which consists of 100 superstars, has half-mass radius 41 kpc and central velocity dispersion 235 km/s. The simulations start from the epoch of maximum expansion. The initial conditions involve a variety of spatial distributions of galaxies, and the velocity dispersion of galaxies as would be permitted for maximum expansion. Dense groups having collapse times shorter than (2/3) H (0) to the -1 are shown to form multiple mergers in a Hubble time H(0) to the -1.From a comparison of the frequencies of cD galaxies, or multiple mergers,in observed and simulated groups, it is concluded that the effective radius of missing halos is less than 41 kpc.

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