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J. A. Hester, D. N. Spergel (Princeton University)
Ram pressure stripping is an important process in the evolution of both dwarf galaxies and large spirals. Large spirals are severely stripped in rich clusters and may be mildly stripped in groups. Dwarf galaxies can be severely stripped in both clusters and groups. A model of ram pressure stripping of a satellite galaxy’s outer H\textsc{i} disk is developed that can be applied to a wide range of environments and satellite galaxy masses. The degree of stripping a satellite experiences is found to depend primarily on the ratio of the satellite galaxy mass to the mass of the host group or cluster. How the effectiveness of stripping depends on the properties of the group and satellite is explored. The model’s predictions are shown to be well matched to H\textsc{i} observations in nearby clusters. Galaxy properties in a sample of groups and poor clusters from the SDSS are compared to galaxy properties in the field and the model is used to explain differences in g-r color between the groups and the field. This project was funded by a NASA Grant.
The author(s) of this abstract have provided an email address for comments about the abstract: jhester@princeton.edu
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.