  The electron population inferred to be responsible for the mini-halo within
the Ophiuchus galaxy cluster is a steep power-law in energy with a slope of
$3.8$. This is substantially different to that predicted by dark matter
annihilation models. In this work we present a method of indirect comparison
between the observed electron spectrum and that predicted for indirect dark
matter emissions. This method utilises differences in the consequences of a
given electron distribution on the subsequent spectral features of synchrotron
emissions. To fully exploit this difference, by leveraging the fact that the
peak and cut-off synchrotron frequencies are substantially different to hard
power-law cases for WIMP masses above $\sim 50$ GeV, we find that we need
$\mu$Jy sensitivities at frequencies above 10 GHz while being sensitive to
arcminute scales. We explore the extent to which this electron spectrum
comparison can be validated with the up-coming ngVLA instrument. We show that,
with the ngVLA, this method allows us to produce far stronger constraints than
existing VLA data, indeed these exceed the Fermi-LAT dwarf searches in a wide
variety of annihilation channels and for all studied magnetic field scenarios.
