  Observations of core-collapse supernovae (CCSNe) reveal a wealth of
information about the dynamics of the supernova ejecta and its composition but
reveal very little direct information about the progenitor star. Constraining
properties of the progenitor and the explosion, such as explosion energy,
requires coupling the observations with a theoretical model of the explosion.
Here, we use a new model for driving turbulence-aided neutrino-driven
core-collapse supernovae in 1D (STIR) which contains a non-parametric treatment
of the neutrino transport while also accounting for turbulence and convection.
We couple this with the SuperNova Explosion Code to produce bolometric light
curves from a landscape of CCSNe driven from self-consistent CCSN simulations
with robust neutrino transport. We compare our results to several well observed
bolometric light curves of Type IIP CCSNe and find that our best fitting models
differ from those found in previous studies using thermal bomb explosions,
indicating ZAMS masses as much as about 10M$_{\odot}$ greater than previous
studies. Using our large sample of 136 self-consistent CCSN explosions, we
explore correlations between observable features of the light curves and
properties of the progenitor star. Among other significant correlations, we
find a robust linear relationship between light curve plateau luminosity and
the iron core mass of the progenitor. This relationship allows for properties
of the core of the progenitor to be constrained for the first time from
photometry alone.
