We present extensive radio observations of a Type Ic supernova , ASASSN-16fp .
Our data represents the lowest frequency observations of the SN beyond 1000 days with a frequency range of 0.33 - 25 GHz and a temporal range of \sim 8 to 1136 days post-explosion .
The observations are best represented by a model of synchrotron emission from a shocked circumstellar shell initially suppressed by synchrotron self-absorption .
Assuming equipartition of energy between relativistic particles and magnetic fields , we estimate the velocity and radius of the blast wave to be v \sim 0.15 c and r \sim 3.4 \times 10 ^ { 15 } cm respectively at t _ { 0 } \sim 8 days post-explosion .
We infer the total internal energy of the radio-emitting material evolves as E \sim 0.37 \times 10 ^ { 47 } ( t/t _ { 0 } ) ^ { 0.65 } erg .
We determine the mass-loss rate of the progenitor star to be \dot { M } \sim ( 0.4 - 3.2 ) \times 10 ^ { -5 } M _ { \odot } yr ^ { -1 } at various epochs post-explosion , consistent with the mass-loss rate of Galactic Wolf-Rayet stars .
The radio light curves and spectra show a signature of density enhancement in the CSM at a radius of \sim 1.10 \times 10 ^ { 16 } cm from the explosion center .