The Carnegie-Irvine Galaxy Survey. VII. Constraints on the Origin of S0
  Galaxies from Their Photometric Structure
  Using high-quality optical images from the Carnegie-Irvine Galaxy Survey, we
perform multi-component decompositions of S0 galaxies to derive accurate
structural parameters to constrain their physical origin. Many S0s do not host
prominent bulges. S0 galaxies have a broad distribution of bulge-to-total
ratios ($B/T$) and S\'ersic indices ($n$), with average values of
$B/T=0.34\pm0.15$ and $n=2.62\pm1.02$, qualitatively consistent with the notion
that S0s define a parallel sequence with and may have evolved from spiral
galaxies. This is further reinforced by the incidence of bars and lenses in
S0s, which when compared with the statistics in spirals, supports the idea that
lenses are demised bars. However, despite their wide range of prominence, the
bulges of S0s form a surprisingly uniform sequence on both the Kormendy and
fundamental plane relations. There is no evidence for population dichotomy or
other indications of differentiation into classical and pseudo bulges. Most of
the S0s reside in the field and in groups; cluster environment is not a
necessary condition for S0 production. The properties of S0 bulges show little
correlation with environmental indicators, after the dependence of galaxy
stellar mass on environment is taken into account. As the bulges of late-type
spirals and S0s are intrinsically different, and environmental effects that may
account for such evolution appear to be minimal, we conclude that late-type
spirals are not plausible progenitors of S0s. The bulges of S0s likely formed
at an early epoch, after which secular processes contributed little to their
subsequent evolution.
