  Previous authors have reported the detection of intrinsically faint sub-mm
emission lensed by the cluster MS0451.6-0305. They suggest that this emission
arises from a merging system composed of a Ly-break galaxy and a pair of
extremely red objects which are multiply-imaged in the optical/NIR
observations. Since the submm emission presents an unusually large angular
extent (~1 arcmin), the possible radio emission asociatted with that system can
help to identify optical/NIR counterparts due to the higher spatial resolution
and astrometric accuracy of the radio observations. Archive VLA data (BnA
configuration at 1.4 GHz) was reduced and analysed. A simple lens model was
constructed to aid the interpretation of the radio and pre-existing sub-mm and
optical/NIR data. We present a 1.4 GHz map of the central region of
MS0451.6-0305 and report the detection of gravitationally lensed radio
emission, coincident with the previously discovered sub-mm lensed emission. The
overall morphology and scale of the radio and sub-mm emission are strikingly
similar, extending ~1 arcmin across the sky. This observation strongly suggests
that the radio and sub-mm emission arise from the same sources. Preliminary
estimates of the total S_850 microns/S_1.4 GHz flux density ratio appear to be
consistent with that expected from distant star forming galaxies. The radio
emission is resolved into 7 distinct components, and the overall structure can
be explained, using a simple lens model, with three multiply-imaged radio
sources at z~2.9. One of these sources is predicted to lie in the middle of the
previously mentioned system in the source plane, suggesting that it is related
to the intense star formation generated during the merging process.
