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For refcode 1992AJ....104..495M:
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1992AJ....104..495M DYNAMICS OF CLUSTERS OF GALAXIES WITH CENTRAL DOMINANT GALAXIES. I. GALAXY REDSHIFTS ELIOT M. MALUMUTH Astronomy Programs, Computer Sciences Corporation, Member GHRS Science Team, Code 681, Goddard Space Plight Canter, Greenbelt, Maryland 20771 GERARD A. KRISS AND W. VAN DYKE DIXON Center for Astrophysical Sciences, The Henry A. Rowland Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, Maryland 21218 HENRY C. FERGUSON Institute of Astronomy, University of Cambridge, The Observatories, Madingley Road, Cambridge CB3 OHA, England CHRISTINE RITCHIE Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218 Received 27 February 1992; revised 27 April 1992 ABSTRACT As part of a study of the dynamical properties of rich clusters with central, dominant D or cD galaxies, we present optical redshifts for a sample of 638 galaxies in the fields of the clusters Abell 85, DC 0107-46, Abell 496, Abell 2052, and DC 1842-63. The velocity histograms and wedge diagrams show evidence for a foreground sheet of galaxies in Abell 85 and background sheets of galaxies in DC 0107-46 and Abell 2052. We have used both the Dressler and Shectman and West and Bothun statistical tests for substructure. We confirm the foreground group projected against the center of Abell 85 found by Beers et al. (1991). We also find significant evidence for substructure in DC 0107-46. We find no evidence of substructure in Abell 496, Abell 2052, and DC 1842-63. The clusters have global velocity dispersions ranging from 551 km s^-1^ for DC 1842-63 to 714 km s^-1^ for A496, and flat dispersion profiles. Mass estimates using the virial theorem and the projected mass method range from 2.3 X 10^14^ M_sun_ for DC 0107-46 to 1.1 X 10^15^ M_sun_ for A85. The velocity of the cD galaxy in each of these clusters with respect to the cluster's velocity ranges from 69 km s^-1^ for A496 to 390 km s^-1^ for A85. When combined with an additional 17 clusters from the literature, cD galaxy peculiar velocities show a positive correlation with Abell richness and with cluster velocity dispersion.
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