  From a diameter-limited sample of 86 `face-on' spiral galaxies, the
bulge-to-disk size and luminosity ratios, and other quantitative measurements
for the prominence of the bulge are derived. The bulge and disk parameters have
been estimated using a seeing convolved Sersic r^(1/n) bulge and a seeing
convolved exponential disk. In general, early-type spiral galaxy bulges have
Sersic values of n>1, and late-type spiral galaxy bulges have values of n<1. In
the B-band, only 8 galaxies have a bulge shape parameter n consistent with the
exponential value of 1, and only 5 galaxies do in the K-band. Application of
the r^(1/n) bulge models results in a larger mean r_e/h ratio for the
early-type spiral galaxies than the late-type spiral galaxies. Although, this
result is shown not to be statistically significant. The mean B/D luminosity
ratio is, however, significantly larger (> 3-sigma) for the early-type spirals
than the late-type spirals. This apparent contradiction with the r_e/h values
can be explained with an iceberg-like scenario, in which the bulges in
late-type spiral galaxies are relatively submerged in their disk. This can be
achieved by varying the relative bulge/disk stellar density while maintaining
the same effective bulge-to-disk size ratio.
  The absolute bulge magnitude - log(n) diagram is used as a diagnostic tool
for comparative studies with dwarf elliptical and ordinary elliptical galaxies.
At least in the B-band, these objects occupy distinctly different regions of
this parameter space. While the dwarf ellipticals appear to be the faint
extension to the brighter elliptical galaxies, the bulges of spiral galaxies
are not.
