  We perform a comparative study between the only radio detected Type I
superluminous supernova (SLSN) PTF10hgi, and the most active repeating fast
radio burst FRB121102. This study has its root in the hypothesized FRB-SLSN
connection that states that magnetars born in SLSN can power FRBs. The wideband
spectrum (0.6--15 GHz) of PTF10hgi presented here, provides strong evidence for
the magnetar wind nebular origin of the radio emission. The same spectrum also
enables us to make robust estimates of the radius and the magnetic field of the
radio emitting region and demonstrates that the nebula is powered by the
rotational energy of the magnetar. This spectrum is then compared with that of
FRB121102 which we extend down to 400 MHz using archival data. The newly added
measurements put very tight constraint on the emission models of the compact
persistent source associated with FRB121102. We find that while both sources
can be powered by the rotational energy of the underlying magnetar, the average
energy injection rate is much higher in FRB121102. Hence, we hypothesise that,
if PTF10hgi is indeed emitting fast radio bursts, those will be much weaker
energetically than those from FRB121102.
