component must be heated continuously by harrasment of more massive cluster galaxies and thus be pressure supported. On the other hand, a variety of observations are available which also support discrepant scenarios of dEs evolution. Recent studies of Virgo cluster dEs [@con03] and also those of the Fornax cluster (see e.g. [@mic04]) have unveiled that a small but significant fraction of them contains gas, has experienced recent SF, and can be argued from internal kinematics and cluster distribution data to represent an infalling class of different types of gas-rich galaxies in or after the state of morphological transformation. Further findings of a significant fraction of rotationally supported dEs in the Virgo cluster [@zee04] and also disk features as e.g. spiral arms and bars [@lis06] support the possibility of morphological transformation from gas-rich progenitor DGs to dEs thru gas exhaustion. Boselli et al. [@bos08a] have comprehensively discussed the different processes of dE origin.

A separation into dE subclasses with respect to their origin should also be visible in an intermediate-age stellar population, blue centers, and flatter figure shape. Indeed, dEs in the Virgo cluster can be divided into different subclasses [@lis07] which differ significantly in their morphology and clustering properties, however, 