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We present a search for late-time rebrightening of radio emission from threesupernovae (SNe) with associated gamma-ray bursts (GRBs). It has beenpreviously proposed that the unusually energetic SNe associated with GRBsshould enter the Sedov-Taylor phase decades after the stellar explosion, andthis SN "remnant" emission will outshine the GRB radio afterglow and bedetectable at significant distances. We place deep limits on the radioluminosity of GRB 980425/SN 1998bw, GRB 030329/SN 2003dh and GRB 060218/SN2006aj, 10-18 years after explosion, with our deepest limit being $L_{\nu}$ $<4 \times 10^{26}$ erg s$^{-1}$ Hz$^{-1}$ for GRB 980425/SN 1998bw. We putconstraints on the density of the surrounding medium for various assumed valuesof the microphysical parameters related to the magnetic field andsynchrotron-emitting electrons. For GRB 060218/SN 2006aj and GRB 980425/SN1998bw, these density limits have implications for the density profile of thesurrounding medium, while the non-detection of GRB 030329/SN 2003dh impliesthat its afterglow will not be detectable anymore at GHz frequencies.

Observational Constraints on Late-Time Radio Rebrightening of GRB-Supernovae