  We investigate the prospects of detecting radio afterglows from long
Gamma-Ray Bursts (GRBs) from Population III (Pop III) progenitors using the SKA
precursor instruments WMA (Murchison Widefield Array) and ASKAP (Australian SKA
Pathfinder). We derive a realistic model of GRB afterglows that encompasses the
widest range of plausible physical parameters and observation angles. We define
the best case scenario of Pop III GRB energy and redshift distributions. Using
probability distribution functions fitted to the observed microphysical
parameters of long GRBs, we simulate a large number of Pop III GRB afterglows
to find the global probability of detection. We find that ASKAP may be able to
detect 35% of Pop III GRB afterglows in the optimistic case, and 27% in the
pessimistic case. A negligible number will be detectable by MWA in either case.
Detections per image for ASKAP, found by incorporating intrinsic rates with
detectable timescales, are as high as $\sim$ 6000 and as low as $\sim$ 11,
which shows the optimistic case is unrealistic. We track how the afterglow flux
density changes over various time intervals and find that, because of their
very slow variability, the cadence for blind searches of these afterglows
should be as long as possible. We also find Pop III GRBs at high redshift have
radio afterglow lightcurves that are indistinguishable from those of regular
long GRBs in the more local universe.
