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The distribution of stars in the Hertzsprung Russell diagram (HRD) for astellar conglomeration represents a snapshot of its evolving stellarpopulation. Some of the supergiant stars may transit the HRD from blue to redand then again to blue during their late evolutionary stages, as exemplified bythe progenitor of SN 1987A. Others may transit a given part of the HRD morethan twice in a "blue loop" and end up as red supergiants before they explode.Since stars in blue loops spend a considerable part of their lives there, thesestages may change the relative number of modeled supergiants in the HRD. Theirlifetimes in turn depend upon the initial mass of the star, how convection inits interior is modeled, and how much mass loss takes place during itsevolution. The observed ratio of the number of blue to red supergiants andyellow to red supergiants sensitively test the stellar evolution theory. Wecompare modeled number ratios of these supergiants with observed data from theLarge Magellanic Cloud as it has a metallicity very similar to that of theenvironment of SN 2013ej. We successfully model these by taking into accountmoderate (exponential) convective overshooting. We explore its effect on thefinal radius and mass of the star prior to core collapse. The radius differsdramatically with overshoot. These factors controlling pre-supernova structuremay affect the post-explosion optical/IR light curves and spectral development.

Type IIP Supernova Progenitors III: Blue to Red Supergiant Ratio in Low Metallicity Models with Convective Overshoot