The environmental dependence of the structure of galactic discs in
  STAGES S0 galaxies: implications for S0 formation
  We present an analysis of V-band radial surface brightness {\mu}(r) profiles
for S0s in different environments using HST/ACS imaging and data from the Space
Telescope A901/2 Galaxy Evolution Survey (STAGES). Using a sample of ~280 field
and cluster S0s, we find that in both environments, ~25 per cent have a pure
exponential disc (Type I) and ~50 per cent exhibit an up-bending disc break
(antitruncation, Type III). However, we find hardly any (< 5 per cent)
down-bending disc breaks (truncations, Type II) in our S0s and many cases (~20
per cent) where no exponential component was observed. We also find no evidence
for an environmental dependence on the disc scalelength or break strength
(outer-to-inner scalelength ratio), implying that the galaxy environment does
not affect the stellar distribution in S0 stellar discs. Comparing disc
structure between these S0s and the spirals from our previous studies, we find:
i) no evidence for the Type I scalelength being dependent on morphology; and
ii) some evidence suggesting the Type II/III break strength is smaller (weaker)
in S0s compared to spirals. Taken together, these results suggest that the
stellar distribution in S0s is not drastically affected by the galaxy
environment. However, some process inherent to the morphological transformation
of spirals into S0s does affect the stellar disc causing a weakening of
{\mu}(r) breaks and may even eliminate truncations from S0s. In further tests,
we perform analytical bulge-disc decompositions on our S0s and compare the
results to those for spirals from our previous studies. For Type III galaxies,
we find that bulge light can account for the excess light at large radii in up
to ~50 per cent of S0s but in only ~15 per cent of spirals. We propose that
this result is consistent with a fading stellar disc (evolving bulge-to-disc
ratio) being an inherent process in the transformation of spirals into S0s.
