  (Abridged) We present a detailed analysis of the morphology, isophotal
parameters and surface brightness profiles for 100 early-type members of the
Virgo Cluster, from dwarfs (M_B = -15.1 mag) to giants (M_B = -21.8 mag). Each
galaxy has been imaged in two filters, closely resembling the Sloan g and z
passbands, using the Advanced Camera for Surveys on board the Hubble Space
Telescope.
  Dust and complex morphological structures are common, with kiloparsec-scale
stellar disks, bars, and nuclear stellar disks seen in 60% of galaxies with
intermediate luminosity (-20 < M_B < -17), and dust seen in 42% of galaxies
brighter than M_B = -18.9 mag. Dust morphologies range from faint wisps and
patches on tens of parsec scales, to regular, highly organized kpc-scale dust
disks, often showing evidence of recent star formation.
  Surface brightness profiles and isophotal parameters are derived typically
within 8 kpc from the center for the brightest galaxies, and 1.5 kpc for the
faintest systems, with a resolution (FWHM) of 7 pc. Based on a parametrization
of the surface brightness profiles in terms of a Sersic or core-Sersic model,
we find that 1) there is no evidence of a bimodal behavior of the slope, gamma,
of the profile in the innermost regions; 2) although the brightest galaxies
have shallow inner profiles, the shallowest profiles (lowest gamma values) are
found in faint dwarf systems; 3) the widely adopted separation of early-type
galaxies between "core" and "power-law" types, which had originally been
prompted by the claim of a clear bimodal distribution of gamma values, is
untenable; and 4) there is no evidence of a structural dichothomy between dwarf
and regular ellipticals.
