  I outline a quantitative method for characterizing galaxies both by
photometric `form' and indices of spectral-type, applicable to both nearby and
distant galaxies. Such a characterization provides insight on galaxy evolution
because there are physical connections between galaxies' stellar populations
and their light distribution. ``Normal'' galaxies' form-parameters
(surface-brightness, image concentration and asymmetry) correlate well with
spectral-index (color), which in turn correlates only weakly with scale (size
or luminosity). Deviations from these normal relations also offer clues to the
physical modes of galaxy formation and evolution. As an example, I contrast a
puzzling, distant population of compact, but luminous, blue, star-forming
galaxies to nearby samples. These distant sources appear to be associated with
the bulk of the luminosity increase since z<1. They have structural properties
comparable to low-redshift populations, and photometric properties within the
norm for nearby, actively star-forming galaxies. When combined, however, their
photometric and structural properties appear to be highly unusual.
