The 'galaxy harassment' model offers an explanation of how the dwarf spiral galaxies in distant clusters, due to encounters with brighter galaxies and the cluster's tidal field, have evolved into today's population of cluster dwarf ellipticals (dEs). We intend to test this model by comparing the metallicity and kinematics of dEs located in the inner and outer regions of the Coma cluster. The model predicts that, on average, dEs located in the inner, high-density cluster regions should be more metallic and have larger velocity dispersions than those in the outer regions. However, no such differences have yet been observed due to a lack of statistically representative samples of cluster dEs that include velocity dispersions and metallicities. To date there are only ∼70 dEs known with these properties, including our sample of ∼50 from the inner 1o region of the Coma cluster. Here we present preliminary results including the kinematic properties of dEs in the central 1o region of the Coma cluster.
American Astronomical Society Meeting Abstracts
- Pub Date:
- December 2003