2016A&A...587A.111A

The surface brightness distribution of ∼30-40% of the early-type dwarf galaxies with -18≤M_B≤-15 in the Virgo and the Coma clusters is fitted by models that include two structural components (Sersic + exponential) as for bright disc galaxies. The goal of the present study is to determine whether early-type dwarf galaxies with a two-component stellar structure in the Virgo and the Coma clusters are low-luminosity copies of bright disc galaxies or are the remnants of bright galaxies strongly transformed by cluster environmental effects. I analysed the location of bright disc galaxies and early-type dwarfs in the r_b,e/h- n plane. The location in this plane of the two-component dwarf galaxies was compared with the remnants of tidally disrupted disc galaxies reported by numerical simulations. Bright unbarred disc galaxies show a strong correlation in the r_b,e/h-n plane. Galaxies with larger Sersic shape parameters show a higher r_b,e/h ratio. In contrast, two-component early-type dwarf galaxies do not follow the same correlation. A fraction (∼55%) of them are located outside the locus defined in this plane by having 95% of bright disc galaxies. This distribution indicates that they are not a low-mass replica of bright disc galaxies. The different location in the r_b,e/h- n plane of two-component early-type dwarfs and bright galaxies can be qualitatively explain whether the former are remnants of disc galaxies strongly transformed by tidal processes. The progenitors of ∼20-25% of early-type dwarf galaxies with -18≤M_B≤-15 in the Virgo and Coma clusters could be bright disc galaxies transformed by effects of the environment. These tidally transformed galaxies can be selected according to their location in the r_b,e/h-n plane.