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For refcode 1995AJ....109..874B:
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1995AJ....109..874B KINEMATICS AND DYNAMICS OF THE MKW/AWM POOR CLUSTERS TIMOTHY C. BEERS AND JEFFREY R. KRIESSLER Electronic mail: beers@msupa.pa.msu.edu; kriessler@msupa.pa.msu.edu CHRISTINA M. BIRD Electronic mail: tbird@kula.phsx.ukans.edu Department of Physics and Astronomy, Michigan State University, E. Lansing, Michigan 48824 JOHN P. HUCHRA Electronic mail: huchra@cfa.harvard.edu Harvard/Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 Received 1994 September 2; revised 1994 November 16 ABSTRACT We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White, and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5 h^-1^ Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km s^-1^, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 <= M/L_B(0)_ <= 200 M_sun_/L_sun_. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.
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