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

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Figure

Fig. 1. Original continuum-subtracted Hα intensity maps used in this study: the LMC on the left (from the SHASSA survey; Gaustad et al
Fig. 3. Hα images of the LMC, with our main-sequence B and O starsamples as well as the SG B[e] stars and LBVs overplotted
Fig. 4. Hα images of the LMC (left) and M 33 (right), with the co-ordinates of our randomly generated uniformly distributed samples ofpositions overplotted.
Table 1. Mean NCRs (⟨NCR⟩) of different stellar types in the LMC at a simulated distance of 20 and 35 Mpc, with accurate coordinates (“acc”)and simulated positional errors of σ = 0.5 arcsec (“err”).
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