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Radial kinematics of isolated elliptical galaxies
Ellipticals in very low-density environments are extremely rare but holdimportant clues about galaxy formation and evolution. In this paper, wecontinue our study of isolated elliptical galaxies, presenting resultson the radial stellar kinematics for 13 isolated early-type galaxies. Wederive radial rotation velocity, velocity dispersion and hermite termsto ~1 effective radius. We observe a dichotomy in kinematic propertiessimilar to that in the elliptical population as a whole, wherelow-luminosity ellipticals tend to be rotationally supported. For allgalaxies the V/σ ratio increases with radius. We findkinematically distinct cores (KDCs), or velocity substructure, in ~40per cent of the galaxies for which we have major axis spectra. Such afraction is similar to that observed for ellipticals in higher-densityenvironments. Most galaxies in the sample reveal kinematic evidence fora nuclear disc. The non-relaxed kinematics in several galaxies suggeststhat they have undergone a merger or accretion event. Isolatedellipticals generally follow the Fundamental Plane defined by clusterellipticals - exceptions being those galaxies with evidence for youngstellar populations. Overall, we find isolated ellipticals have similarkinematic properties to their counterparts in higher-densityenvironments.
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Observation and Astrometry data
| Constellation: | Fluss Eridanus |
| Right ascension: | 02h30m37.17s |
| Declination: | -47°55'52.4" |
| Apparent magnitude: | 8.529 |
| Distance: | 877.193 parsecs |
| Proper motion RA: | 5 |
| Proper motion Dec: | 0 |
| B-T magnitude: | 10.218 |
| V-T magnitude: | 8.669 |
Catalogs and designations:
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