  We present a panchromatic study of nearby starburst galaxies from the
ultraviolet to the visible, including narrow band H(alpha) using WIYN and HST
data, to determine how star formation processes affect the morphology and
integrated fluxes of nearby starbursts. We find the UV/H(alpha) morphology of
starbursts tend to differ, although not in a standard or predictable manner.
  From our sample of six nearby starbursts, three systems show a good
correlation between UV and H(alpha) fluxes, but we find differences in UV and
H(alpha) morphology between the other three. Occasionally we find systems with
well defined H II regions without the corresponding brightness in the UV, and
vice-versa. We discuss the likely mechanisms behind these differences which
include: starburst ages, dust absorption, stellar energy ejecta through SNe and
winds, as well as leakage of UV photons from stellar clusters. We conclude that
the large scale morphological features in starbursts are primarily due to both
age and absorption from a `picket fence' dust distribution.
  We further demonstrate the similarity and differences between these nearby
starbursts and high redshift star forming galaxies. The overall morphology of
our sample of starbursts changes little between UV and visible wavelengths. If
high redshift galaxies are similar to these starbursts, their morphologies
should change little between rest-frame UV and optical. We also show that FIR
and UV spectral energy distributions and slopes can be used to determine large
scale morphological features for extreme starbursts, with the steepest FIR
slopes correlating with the most disturbed galaxies.
