  We have derived the photometric parameters for the structural components of a
sample of fourteen SB0 galaxies by applying a parametric photometric
decomposition to their observed $I$-band surface brightness distribution.
  We find that SB0 bulges are similar to bulges of the early-type unbarred
spirals, i.e. they have nearly exponential surface brightness profiles
($<n>=1.48\pm0.16$) and their effective radii are strongly coupled to the scale
lengths of their surrounding discs ($<r_e/h>=0.20\pm0.01$). The photometric
analysis alone does not allow us to differentiate SB0 bulges from unbarred S0
ones.
  However, three sample bulges have disc properties typical of pseudobulges.
The bulges of NGC 1308 and NGC 4340 rotate faster than bulges of unbarred
galaxies and models of isotropic oblate spheroids with equal ellipticity. The
bulge of IC 874 has a velocity dispersion lower than expected from the
Faber--Jackson correlation and the fundamental plane of the elliptical galaxies
and S0 bulges. The remaining sample bulges are classical bulges, and are
kinematically similar to lower-luminosity ellipticals. In particular, they
follow the Faber--Jackson correlation, lie on the fundamental plane and those
for which stellar kinematics are available rotate as fast as the bulges of
unbarred galaxies.
