  We present a quantitative analysis of the morphologies for 199 nearby
galaxies as parameterized with measurements of the concentration, asymmetry,
and clumpiness (CAS) parameters at wavelengths from 0.15-0.85 micrometers. We
find that these CAS parameters depend on both galaxy type and the wavelength of
observation. As such, we use them to obtain a quantitative measure of the
"morphological k-correction", i.e., the change in appearance of a galaxy with
rest-frame wavelength. Whereas early-type galaxies (E--S0) appear about the
same at all wavelengths longward of the Balmer break, there is a mild but
significantly-determined wavelength-dependence of the CAS parameters for
galaxies types later than S0, which generally become less concentrated, and
more asymmetric and clumpy toward shorter wavelengths. Also, as a merger
progresses from pre-merger via major-merger to merger-remnant stages, it
evolves through the CAS parameter space, becoming first less concentrated and
more asymmetric and clumpy, and then returning towards the "locus" of normal
galaxies. The final merger products are, on average, much more concentrated
than normal spiral galaxies.
