  Ultraviolet Luminous Galaxies (UVLGs) have been identified as intensely
star-forming, nearby galaxies. A subset of these, the supercompact UVLGs, are
believed to be local analogs of high redshift Lyman Break Galaxies. Here we
investigate the radio continuum properties of this important population for the
first time. We have observed 42 supercompact UVLGs with the VLA, all of which
have extensive coverage in the UV/optical by GALEX and SDSS. Our analysis
includes comparison samples of multiwavelength data from the Spitzer First Look
Survey and from the SDSS-Galex matched catalogs. In addition we have Spitzer
MIPS data for 24 of our galaxies and find that they fall on the radio-FIR
correlation of normal star-forming galaxies. We find that our galaxies have
lower radio-to-UV ratios and lower Balmer decrements than other local galaxies
with similar (high) star formation rates. Optical spectra show they have lower
Dn(4000) and HdeltaA indices, higher Hbeta emission-line equivalents widths,
and higher [OIII]5007/Hbeta emission-line ratios than normal star forming
galaxies. Comparing these results to galaxy spectral evolution models we
conclude that supercompact UVLGs are distinguished from normal star forming
galaxies firstly by their high specific star formation rates. Moreover,
compared to other types of galaxies with similar star formation rates, they
have significantly less dust attenuation. In both regards they are similar to
Lyman Break Galaxies. This suggests that the process that causes star formation
in the supercompact UVLGs differs from other local star forming galaxies, but
may be similar to Lyman Break Galaxies.
