  We compare optical and near-infrared colors of disks and bulges in a
diameter-limited sample of inclined, bright, nearby, early-type spirals. Color
profiles along wedge apertures at 15 degree from the major axis and on the
minor axis on the side of the galaxy opposite to the dust lane are used to
assign nominal colors for the inner disks (at 2 scale length) and for the
bulges (~ 0.5 r_eff), respectively. We estimate that the effects of dust
reddening and the cross-talk between the colors of the two components is
negligible. We find that color differences (bulge -- disk) are very small:
Delta(U-R)=0.126 +/- 0.165, Delta(R-K)=0.078 +/- 0.165. Disks tend to be bluer
by an amount three times smaller than that reported by Bothun & Gregg (1990)
for S0's. Color variations from galaxy to galaxy are much larger than color
differences between disk and bulge in each galaxy. Probably, the underlying old
population of disks and bulges is much more similar than the population
paradigm would lead us to believe. Implied age differences, assuming identical
metallicities, are less than 30%.
