Isophotal maps of the WFPC2 and ACS images of our target galaxies within a FoV of 20 × 20″. In the bottom right of each panel we show a cut out of the central 3 × 3″. The contours of our best-fitting MGE model (red) are superimposed on the HST images. For the models, foreground stars and close galaxies were masked. For NGC 2784, NGC 4281, and NGC 7049 a dust correction of the internal dust rings had to be applied before MGE modeling their surface brightness. The MGE models were build from the combined photometric information of HST (r <  10″) and wide FoV data (r >  10″) from ATLAS^3D and the CGS (Ho et al. 2011) survey.