do not show any central clustering, but are distributed more like the late-type galaxies. These types of dEs show different disk signatures, such as bars and spiral structures, are not spheroidal, but rather thick disk-like galaxies. Similar shapes were also found for the brighter, non-nucleated dEs. There is only a small fraction of nucleated dEs whithout any disk features or cores, which keep the image of spheroidal objects consisting of old stars.

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\[fig:VCdE\]

A figure analysis of Virgo dEs correlates with the averaged orbit velocity in the sense that flatter dEs show on average a larger orbital velocity (700 km/s) than those originating within the cluster (300 km/s) [@lis09] (see Fig. 4). This kinematical dichotomy is expected because galaxies formed in virial equilibrium within the cluster retain their initial kinetic energy while the cluster mass grew. Galaxies falling into the present cluster potential must therefore possess larger velocities. To obtain information about both evolutionary stages, the young infalling vs. the late cluster members, [@got09] studied SDSS data. The basic model is that dIrrs which are formed outside the Virgo Cluster and becoming stripped on their infall, by this being transformed into dEs, should reveal properties recognizably different from 