  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 $v \sim 0.15c$ 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 $\dot{M}$ $\sim$ $(0.4-3.2) \times10^{-5}$
$M_{\odot}\rm yr^{-1}$ 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.
