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We revisit the exquisite archival radio data for the Type Ic supernova SN1994I and present a revised model for the SN radio emission and a pilot studythat aims to constrain the rate of C-band radio transients within the face-onhost galaxy, M51 (NGC 5194). We find that the temporal and spectral evolutionof the SN\,1994I radio emission are well fit by a synchrotron self-absorptionmodel and use this to estimate physical parameters. We compute a pre-explosionmass loss rate of $\dot{M}=3.0 \times 10^{-5} M_{\odot}$ yr$^{-1}$ for theprogenitor, consistent with those observed from galactic Wolf-Rayet stars. Ourmodel makes different assumptions for the dynamical model for the shockwaveinteraction than the model previously published by \cite{weil11}, but our$\dot{M}$ is consistent with theirs to within errors and assumptions. Drawingfrom a subset of the archival radio observations from the Very Large Arraycollected for the monitoring of SN\,1994I, we conduct a pilot study to searchfor previously-unidentified transients. Data were primarily taken at afrequency of 4.9 GHz and are logarithmic in cadence, enabling sensitivity totransients with variability timescales ranging from days to months. We find nonew transient detections in 31 epochs of data, allowing us to place a $2\sigma$upper limit of 17 deg$^{-2}$ for the source density of radio transients above0.5 mJy ($L\gtrsim4\times10^{25}$ erg s$^{-1}$ Hz$^{-1}$ at the distance ofM51). This study highlights the feasibility of utilizing archival high-cadenceradio studies of supernova host galaxies to place constraints on the radiotransient rate as a function of luminosity in the local Universe.

A New Model for the Radio Emission from SN 1994I and an Associated Search for Radio Transients in M51