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We study the spatial correlations between the H$\alpha$ emission anddifferent types of massive stars in two local galaxies, the Large MagellanicCloud (LMC) and Messier 33. We compare these to correlations derived forcore-collapse supernovae (CCSNe) in the literature to connect CCSNe ofdifferent types with the initial masses of their progenitors and to test thevalidity of progenitor mass estimates which use the pixel statistics method. Weobtain samples of evolved massive stars in both galaxies from catalogues withgood spatial coverage and/or completeness, and combine them with coordinates ofmain-sequence stars in the LMC from the SIMBAD database. We calculate thespatial correlation of stars of different classes and spectral types withH$\alpha$ emission. We also investigate the effects of distance, noise andpositional errors on the pixel statistics method. A higher correlation withH$\alpha$ emission is found to correspond to a shorter stellar lifespan, and weconclude that the method can be used as an indicator of the ages, and thereforeinitial masses, of SN progenitors. We find that the spatial distributions oftype II-P SNe and red supergiants of appropriate initial mass ($\gtrsim$9$M_{\odot}$) are consistent with each other. We also find the distributions oftype Ic SNe and WN stars with initial masses $\gtrsim$20 $M_{\odot}$consistent, while supergiants with initial masses around 15 $M_{\odot}$ are abetter match for type IIb and II-L SNe. The type Ib distribution corresponds tothe same stellar types as type II-P, which suggests an origin in interactingbinaries. On the other hand, we find that luminous blue variable stars show amuch stronger correlation with H$\alpha$ emission than do type IIn SNe.

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies