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Current population synthesis modeling suggests that 30-50% of Type IIsupernovae originate from binary progenitors, however, the identification of abinary progenitor is challenging. One indicator of a binary progenitor is thatthe surrounding stellar population is too old to contain a massive singlestar.Measurements of the progenitor mass of SN 2017eaw are starkly dividedbetween observations made temporally close to core-collapse which show aprogenitor mass of 13-15 solar masses (final helium core mass of 4.4 to 6.0solar masses - which is a more informative property than initial mass) andthose from the stellar population surrounding the SN which find M<10.8 solarmasses (helium core mass <3.4 solar masses). In this paper, we reanalyze thesurrounding stellar population with improved astrometry and photometry, findinga median age of 16.8 (+3.2, -1.0) Myr for all stars younger than 50 Myr (heliumcore mass of 4.7 solar masses) and 85.9 (+3.2, -6.5) Myr for stars younger than150 Myr. 16.8 Myr is now consistent with the helium core mass range derivedfrom the temporally near explosion observations for single stars. Applying thecombined constraints to population synthesis models, we determine that theprobability of the progenitor of SN 2017eaw being an initially single-star is65% compared to 35% for prior binary interaction. 85.9 Myr is inconsistent withany formation scenarios. We demonstrate that combining progenitor ageconstraints with helium core mass estimates from red supergiant SED modeling,late-time spectra, and indirectly from light curve modeling can help todifferentiate single and binary progenitor scenarios and provide a frameworkfor the application of this technique to future observations.

Considering the Single and Binary Origins of the Type IIP SN 2017eaw