KINEMATIC PROPERTIES AS PROBES OF THE EVOLUTION OF DWARF GALAXIES IN THE VIRGO CLUSTER
- Universidad Complutense de Madrid, 28040, Madrid (Spain)
- Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS, 38 rue F. Joliot-Curie, 13388 Marseille (France)
- Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen (Netherlands)
- Instituto de Astrofisica de Canarias, E-38200, La Laguna, Tenerife (Spain)
- Max-Planck-Institut fuer Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching (Germany)
- Centro Astronomico Hispano Aleman, Calar Alto (CSIC-MPG), AlmerIa (Spain)
We present new observational results on the kinematical, morphological, and stellar population properties of a sample of 21 dEs located both in the Virgo Cluster and in the field, which show that 52% of the dEs (1) are rotationally supported, (2) exhibit structural signs of typical rotating systems such as disks, bars, or spiral arms, (3) are younger (approx3 Gyr) than non-rotating dEs, and (4) are preferentially located either in the outskirts of Virgo or in the field. This evidence is consistent with the idea that rotationally supported dwarfs are late-type spirals or irregulars that recently entered the cluster and lost their gas through a ram pressure stripping event, quenching their star formation and becoming dEs through passive evolution. We also find that all, but one, galaxies without photometric hints for hosting disks are pressure supported and are all situated in the inner regions of the cluster. This suggests a different evolution from the rotationally supported systems. Three different scenarios for these non-rotating galaxies are discussed (in situ formation, harassment, and ram pressure stripping).
- OSTI ID:
- 21389335
- Journal Information:
- Astrophysical Journal (Online), Vol. 707, Issue 1; Other Information: DOI: 10.1088/0004-637X/707/1/L17; ISSN 1538-4357
- Country of Publication:
- United States
- Language:
- English
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