  Multiple astrophysical probes of the cosmic star formation history yield
widely different inferences of this rate at redshifts z > 1. While all probes
seem to indicate a period of peak star formation known as the cosmic noon
between 1.5 < z < 3, the detailed inferences from these probes are in
disagreement. In particular, the magnitude of the peak star formation rate
density indicated by H-alpha data is higher by a factor of ~ 4 compared to the
magnitude of the peak indicated by UV/IR data. In this work, we explore the
potential of future measurements of the diffuse supernova neutrino background
at the Hyper-Kamiokande (HK) experiment to resolve the discrepancy and help pin
down the magnitude of the peak cosmic star formation rate. We find that,
depending upon the cosmic core-collapse supernova neutrino spectrum, HK loaded
with 0.1% Gadolinium by mass has the potential to discriminate between the
different star formation histories with between 1.6-20 years of data
collection.
