  We use the results of a supernova light-curve population synthesis to predict
the range of possible supernova light curves arising from a population of
single-star progenitors that lead to type IIP supernovae. We calculate multiple
models varying the initial mass, explosion energy, nickel mass and nickel
mixing and then compare these to type IIP supernovae with detailed light curve
data and pre-explosion imaging progenitor constraints. Where a good fit is
obtained to observations, we are able to achieve initial progenitor and nickel
mass estimates from the supernova lightcurve that are comparable in precision
to those obtained from progenitor imaging. For two of the eleven IIP supernovae
considered our fits are poor, indicating that more progenitor models should be
included in our synthesis or that our assumptions, regarding factors such as
stellar mass loss rates or the rapid final stages of stellar evolution, may
need to be revisited in certain cases. Using the results of our analysis we are
able to show that most of the type IIP supernovae have an explosion energy of
the order of log(E_exp/ergs)=50.52+/-0.10 and that both the amount of nickel in
the supernovae and the amount of mixing may have a dependence on initial
progenitor mass.
