  The study of gamma-ray burst (GRB) host galaxies in the radio, sub-mm, and
X-ray wavelength regimes began only recently, in contrast to optical studies.
This is mainly due to the long timescale on which the radio afterglow emission
decays, and to the intrinsic faintness of radio emission from star-forming
galaxies at z~1, as well as source confusion in sub-mm observations; X-ray
observations of GRB hosts have simply not been attempted yet. Despite these
difficulties, we have recently made the first detections of radio and sub-mm
emission from the host galaxies of GRB980703 and GRB010222, respectively, using
the VLA and the SCUBA instrument on JCMT. In both cases we find that the
inferred star formation rates (~500 solar masses per year) and bolometric
luminosities (~few 10^12 solar luminosities) indicate that these galaxies are
possibly analogous to the local population of Ultra-Luminous Infrared Galaxies
(ULIRGs) undergoing a starburst. However, there is a modest probability that
the observed emission is due to AGN activity rather than star formation, thus
requiring observations with Chandra or XMM. The sample of GRB hosts offers a
number of unique advantages to the broader question of the evolution of
galaxies and star formation from high redshift to the present time since: (i)
GRBs trace massive stars, (ii) are detectable to high redshifts, and (iii) have
immense dust penetrating power. Therefore, radio/sub-mm/X-ray observations of
GRB hosts can potentially provide crucial information both on the nature of the
GRB host galaxies, and on the history of star formation.
