Constraining Core-Collapse Supernova Theory with Progenitor Masses
Abstract
A fundamental prediction of stellar evolution theory is that the explosive fates of massive stars is determined by its zero-age-main-sequence mass. In particular, theory predicts that single stars above about 8 solar masses (M⊙) eventually collapse, but it is not clear if every core collapse leads to explosion. Recent investigations suggest that lower mass stars may explode more easily than higher mass stars, with the latter being more likely to collapse directly into a black hole. To test these basic predictions, we developed a hierarchical Bayesian model, to infer the parameters of the progenitor age distribution. In particular, we infer the age of stellar populations surrounding 94 supernova remnants (SNRs) in M31 and M33. From these ages, we infer the progenitor mass distribution. Assuming each progenitor evolved as a single star, we infer a minimum mass for explosion of 7.33+0.02-0.16 M⊙, a power-law distribution with a slope of -2.96+0.45-0.25, and the maximum mass is > 59 M⊙. These inferred parameters are consistent with previous estimates using direct detections and the age-dating technique. However, the primary difference is that the statistical uncertainty is a factor of ~10 smaller. Since the age-dating technique does not require precursor imaging, it expands the number of progenitor estimates to many more core collapse supernovae (CCSNe) and hundreds of SNRs. In this talk, we introduce new results for 200 SNRs in M83, discuss how these results impact CCSN theory, discuss potential biases, and how future work may mitigate these biases.
- Publication:
-
American Astronomical Society Meeting Abstracts #235
- Pub Date:
- January 2020
- Bibcode:
- 2020AAS...23525102D