The kinematics of dense clusters of galaxies. I - The data

Details The kinematics of dense clusters of galaxies. I - The data The kinematics of dense clusters of galaxies. I - The data

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....106.1273z&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 106, no. 4, p. 1273-1300.

Astronomy and Astrophysics

Astronomy

113

Dark Matter, Galactic Clusters, Red Shift, Velocity Distribution, Astronomical Models, Galactic Rotation, Galactic Structure

Scientific paper

We have measured redshifts in the fields of the 31 R greater than 1 Abell clusters with z of 0.02-0.05 and absolute b exp II above 30 deg. At least ten of the fields are severely contaminated by superimposed velocity peaks. We derive the mean velocities and velocity dispersions of the 25 dense peaks in the sample. The abundance of peaks, 6.6 x 10 exp -6 h-cubed Mpc exp -3, is consistent with the mean number density of R above 1 Abell clusters. The range of velocity dispersions is 304-1346 km/s. The median dispersion is 718 km/s. The subset of eight systems with cD galaxies has a median velocity dispersion of 792 km/s, close to that of non-cD systems (626 km/s). When these data are combined with 16 cD cluster velocity dispersions from our previous study (Zabludoff et al., 1990, or ZHG) and Dunn (1991), eight of 25 cD galaxies have peculiar motions larger than half the cluster velocity dispersions. These findings further support the conclusions of Beers and Geller (1983), ZHG, and Dunn (1991), who argue that cD galaxies do not lie in the global kinematic center, but in local potential minima. If so, systems with speeding cD's are probably a guide to substructure in dynamically evolving systems.

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