Core-collapse supernovae ages and metallicities from emission-line diagnostics of nearby stellar populations

TL;DR

This study uses emission-line diagnostics and stellar population models to analyze the ages and metallicities of stars associated with nearby core-collapse supernovae, revealing insights into their progenitors and host environments.

Contribution

It introduces a comparison of single star and binary star models for CCSN host environments, highlighting the importance of binary interactions for accurate metallicity estimates.

Findings

Binary-star models fit observed data better.

Type II and Ibc SNe progenitors have similar ages.

Lower metallicity environments favor Type II supernovae.

Abstract

Massive stars are the main objects that illuminate H II regions and they evolve quickly to end their lives in core-collapse supernovae (CCSNe). Thus it is important to investigate the association between CCSNe and H II regions. In this paper, we present emission line diagnostics of the stellar populations around nearby CCSNe, that include their host H II regions, from the PMAS/PPAK Integral-field Supernova hosts COmpilation (PISCO). We then use BPASS stellar population models to determine the age, metallicity and gas parameters for H II regions associated with CCSNe, contrasting models that consider either single star evolution alone or incorporate interacting binaries. We find binary-star models, that allow for ionizing photon loss, provide a more realistic fit to the observed CCSN hosts with metallicities that are closer to those derived from the oxygen abundance in O3N2. We also find that type II and type Ibc SNe arise from progenitor stars of similar age, mostly from 7 to 45 Myr, which corresponds to stars with masses < 20 solar mass . However these two types SNe have little preference in their host environment metallicity measured by oxygen abundance or in progenitor initial mass. We note however that at lower metallicities supernovae are more likely to be of type II.