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There is observational evidence of a dearth in core-collapse supernova (ccSN)explosions from stars with zero age main sequence (ZAMS) mass M_0~17-30 Msol,referred to as the 'red supergiant problem'. However, simulations now predictthat above 20Msol we should indeed only expect stars within certain pockets ofM_0 to produce a visible SN explosion. Validating these predictions requireslarge numbers of ccSNe of different types with measured M_0, which ischallenging. In this paper we explore the reliability of using host galaxyemission lines and the Halpha equivalent width to constrain the age, and thusthe M_0 of ccSNe progenitors. We use Binary Population and Spectral Synthesismodels to infer a stellar population age from MUSE observations of the ionisedgas properties and Halpha EW at the location of eleven ccSNe with reliable M_0measurements. Comparing our results to published M_0 values, we find thatmodels that do not consider binary systems yield stellar ages that aresystematically too young (thus M_0 too large), whereas accounting for binarysystem interactions typically overpredict the stellar age (thus underpredictM_0). Taking into account the effects of photon leakage bring our M_0 estimatesin much closer agreement with expectations. These results highlight the needfor careful modelling of diffuse environments, such as are present in thevicinity of type II SNe, before ionised emission line spectra can be used asreliable tracers of progenitor stellar age.

The 50-100pc scale parent stellar populations of type II supernovae and limitations of single star evolution models