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Kinematics and dynamics of the haloes of supergiant galaxies
Measurements of the internal kinematics of the haloes of threesupergiant (cD or giant dumbbell) galaxies in moderately rich clustersare presented. It is found that these galaxies have velocity dispersionprofiles which are flat or which rise with increasing radius. Theobservations are explained by two simple models. The first class hasisotropic velocity dispersions and a two-component mass distribution: abright component with a density distribution which follows a King model,and a dark isothermal component with a density distribution which isslightly more concentrated than that of the galaxies in the cluster as awhole. The second class has predominantly tangential motions in the haloof the galaxy and no dark component. In common with most luminouselliptical galaxies these supergiant galaxies are not flattered byrotation. In the two dumbbells studied the relative velocities betweenthe nuclei are comparable to the stellar velocity dispersions in the cDenvelopes.
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Observation and Astrometry data
| Constellation: | エリダヌス座 |
| Right ascension: | 02h01m55.03s |
| Declination: | -50°07'38.0" |
| Apparent magnitude: | 7.809 |
| Distance: | 287.356 parsecs |
| Proper motion RA: | 26.7 |
| Proper motion Dec: | 36.1 |
| B-T magnitude: | 8.949 |
| V-T magnitude: | 7.904 |
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