[Previous] | [Session 5] | [Next]
C.J. Conselice, J.S. Gallagher (University of Wisconsin-Madison), R.F.G. Wyse (Johns Hopkins University)
The Perseus cluster provides an opportunity to investigate dwarf ellipticals and spheroidals in a relatively nearby, rich cluster of galaxies. We present the results of a study on these early type dwarf galaxies using both high resolution (0.6''-0.8'' seeing) deep WIYN images of color structures of the Perseus dwarfs, as well as wide-field data from the KPNO 0.9m. These images are analyzed to provide information on global properties of dE and dSph galaxies in the Perseus cluster; including integrated magnitudes, (B-R) colors, and to explore their internal structures (asymmetries, concentrations, color gradients). We find significant structural differences between the dwarfs found in the Perseus and the otherwise similar Coma cluster. The dwarfs in Perseus appear to be much more regular and symmetric, and less disturbed than do the Coma cluster dwarfs. We also show the differences between the Perseus dwarf population as a function of location within the cluster, and discuss how these observations constrain models that explain the large population of these fragile objects in the intense gravitational gradients of cluster environments.
If the author provided an email address or URL for general inquiries, it is a
s follows: