  The detailed study of supernovae (SNe) and their progenitors allows to better
understand the evolution of massive stars and how these end their lives.
Despite its importance, the range of physical parameters for the most common
type of explosion, the type II supernovae (SNe II), is still unknown. In
particular, previous studies of type II-Plateau supernovae (SNe II-P) showed a
discrepancy between the progenitor masses inferred from hydrodynamic models and
those determined from the analysis of direct detections in archival images. Our
goal is to derive physical parameters (progenitor mass, radius, explosion
energy and total mass of nickel) through hydrodynamical modelling of light
curves and expansion velocity evolution for a select group of 6 SNe II-P (SN
2004A, SN 2004et, SN 2005cs, SN 2008bk, SN 2012aw, and SN 2012ec) that
fulfilled the following three criteria: 1) they have enough photometric and
spectroscopic monitoring to allow for a reliable hydrodynamical modelling; 2)
there is a direct progenitor detection; and 3) there is a confirmation of the
progenitor identification via its disappearance in post-explosion images. We
then compare the masses obtained by our hydrodynamic models with those obtained
by direct detections of the progenitors to test the existence of such a
discrepancy. As opposed to some previous works, we find a good agreement
between both methods.

Solar and Stellar Astrophysics;High Energy Astrophysical Phenomena