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Date and Time of the Query: 2019-05-25 T23:05:25 PDT
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For refcode 1991A&A...246..349B:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
1991A&A...246..349B Internal stellar kinematics of three dwarf ellipticals in the Local Group R. Bender, A. Paquet, and J.-L. Nieto Landessternwarte Konigstuhl, W-6900 Heidelberg 1, Federal Republic of Germany Department of Physics, Oxford University, Keble Road, Oxford OX1 3RH, England Observatoire Midi-Pyrenees, Unite Associee au CNRS 285, 14, Ave. Edouard- Belin, F-34100 Toulouse, France Canada-France-Hawaii Telescope Corporation, PO. Box 1597, Kamuela. HI 96743, U.S.A. Received January 17, accepted March 6, 1991 Abstract. Rotation curves for the stellar bodies of three low surface- brightness dwarf ellipticals in the Local Group are presented (NGC 147, NGC 185, NGC 205). NGC 147 rotates with 6.5 +/- 2 km/s and has a mean velocity dispersion of 23 +/- 5 km/s between 20 arcsec and 100 arcsec; this galaxy is the faintest one for which a well sampled stellar rotation curve has been measured so far. NGC 185 and NGC 205 show no significant rotation (< 3 km/s). In NGC 205 it is indicated that the rotation may reverse at about 40 arcsec distance from the center; in addition. the velocity dispersion rises radially. Both effects most likely reflect the tidal interaction with M 31. The previous velocity dispersion measurements of NGC 205 are confirmed (~40 - 50 km/s outside the nucleus), the velocity dispersion of NGC 185 is similar to the one of NGC 147 (23 +/-5 km/s). The fact that none of the three objects is rotationally flattened represents further strong evidence that low surface-brightness-dwarf ellipticals may be in general anisotropic systems. It is speculated that the anisotropy of these galaxies may be due to galactic winds and the fact that the molecular cloud-systems out of which they were formed could not dissipate and relax as efficiently as it was the case in low- luminosity compact ellipticals. Blue mass-to-light ratios were derived using King's method. We obtained similar values for all three galaxies of M/L_B_~7 in solar units. These have to be taken with some care, however, because of the objects' anisotropic velocity distributions. Key words: dwarf elliptical galaxies, kinematics of galaxies
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