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 _ { \mathrm { exp } } /ergs ) =50.52 \pm 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 .