  The rate of gravitational collapse (type II) supernovae in our galaxy is
uncertain by a factor of three or more. One way to determine the galactic
supernova rate is through a radiogeochemical experiment (for example, the
molybdenum-technetium experiment) that would integrate the neutrino flux over
several million years. While such a measurement is designed to integrate the
flux over the entire galaxy, nearby star-forming regions could skew the
results. We model the flux from a recently identified such region, the
Scorpius-Centaurus OB association, and compare with the flux from the rest of
the galaxy.
