  We infer the progenitor mass distribution for 22 historic core-collapse
supernovae (CCSNe) using a Bayesian hierarchical model. For this inference, we
use the local star formation histories to estimate the age for each supernova
(SN). These star formation histories often show multiple bursts of star
formation; our model assumes that one burst is associated with the SN
progenitor and the others are random bursts of star formation. The primary
inference is the progenitor age distribution. Due to the limited number of
historic SNe and highly uncertain star formation at young ages, we restrict our
inference to the slope of the age distribution and the maximum age for CCSNe.
Using single-star evolutionary models, we transform the progenitor age
distribution into a progenitor mass distribution. Under these assumptions, the
minimum mass for CCSNe is ${M_\textrm{min}}~=~8.60^{+0.37}_{-0.41} \ M_\odot$
and the slope of the progenitor mass distribution is $\alpha =
-2.61^{+1.05}_{-1.18}$. The power-law slope for the progenitor mass
distribution is consistent with the standard Salpeter initial mass function
($\alpha = -2.35$). These values are consistent with previous estimates using
precursor imaging and the age-dating technique, further confirming that using
stellar populations around SN and supernova remnants is a reliable way to infer
the progenitor masses.
