Early-type dwarf galaxies with multicomponent stellar structure: Are
  they remnants of disc galaxies strongly transformed by their environment?
  The surface brightness distribution of $\sim$30-40$\%$ of the early-type
dwarf galaxies with $-18 \leq M_{B} \leq -15$ in the Virgo and the Coma
clusters is fitted by models that include two structural components (S\`ersic +
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 S\`ersic 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 ($\sim$55%) of them are located outside the locus
defined in this plane by having 95$\%$ 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 $\sim$20-25% of early-type dwarf galaxies with
$-18 \leq M_{B} \leq -15$ 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.
