dEs which have already aged in the cluster, as e.g. colors, effecitve radius, radial stellar distribution, and abundances. One result by [@got09] is that for the two dE populations, with and without cores, distinguished by their Sersic parameter, there is only a slight indication that non-nucleated dEs are more concentrated towards the inner cluster regions, whereas the fraction of nuclated dE is randomly distributed, while [@lis07] found it to increase with distance. An analysis of the relation between the central surface brightness and the Sersic parameter shows the expected tendency to higher values for brighter galaxies. Furthermore, there were no further relations found of the Sersic parameter, the effective radius, or the distance from M 87.

Deeper insights are provided by spectra. Koleva et al. [@kol09] found most dEs in the Fornax cluster to be roundish and to contain significant metallicity gradients already in the old stellar population. They argue that this is due to a lack of sufficient mixing. In contrast, rotationally supported dEs have flat metallicity distributions. Compared with simulations this can be attributed to galactic winds, but the picture of metallicity and gradients is not yet clear. While [@spo09] show a tight positive correlation between the total 