  Since 1997 the afterglow of gamma-ray bursting sources (GRBs) has
occasionally been detected in the radio, as well in other wavelengths bands. In
particular, the interesting and unusual gamma-ray burst GRB980425, thought to
be related to the radio supernova SN1998bw, is a possible link between the two
classes of objects. Analyzing the extensive radio emission data avaliable for
SN1998bw, one can describe its time evolution within the well established
framework available for the analysis of radio emission from supernovae. This
then allows relatively detailed description of a number of physical properties
of the object. The radio emission can best be explained as the interaction of a
mildly relativistic shock with a dense preexplosion stellar wind-established
circumstellar medium (CSM) that is highly structured both azimuthally, in
clumps or filaments, and radially, with observed density enhancements. Because
of its unusual characteristics for a Type Ib/c supernova, the relation of
SN1998bw to GRB980425 is strengthened and suggests that at least some classes
of GRBs originate in supernova (SN) massive star explosions. Thus, employing
the formalism for describing the radio emission from supernovae (SNe) and
following the link through SN1998bw/GRB980425, it is possible to model the
gross properties of the radio and optical/infrared (OIR) emission from the
half-dozen GRBs with extensive radio observations. From this we conclude that
at least some members of the ``slow-soft'' class of GRBs can be attributed to
the explosion of a massive star in a dense, highly structured CSM that was
presumably established by the preexplosion stellar system.
