Core-Collapse Supernova Rate Synthesis Within 11 Mpc

TL;DR

This study compares observed supernova rates in nearby galaxies with simulated predictions using binary star models, revealing insights into star formation history and supernova type ratios within 11 Mpc.

Contribution

It introduces binary population synthesis into supernova rate modeling, improving the match with observed supernova type ratios and star formation histories.

Findings

Binary stars increase predicted Type Ibc supernovae rates.

Star formation peaked over 3 million years ago in best-fit models.

Binary inclusion has little effect on total CCSN rate.

Abstract

The 11 Mpc H-alpha and Ultraviolet Galaxy (11HUGS) Survey traces the star formation activity of nearby galaxies. In addition within this volume the detection completeness of core-collapse supernovae (CCSNe) is high therefore by comparing these observed stellar births and deaths we can make a sensitive test of our understanding of how stars live and die. In this paper, we use the results of the Binary Population and Spectral Synthesis (BPASS) code to simulate the 11HUGS galaxies H-alpha and far-ultraviolet (FUV) star formation rate indicators (SFRIs) and simultaneously match the core-collapse supernova (CCSN) rate. We find that stellar population including interacting binary stars makes little difference to the total CCSN rate but increases the H-alpha and FUV fluxes for a constant number of stars being formed. In addition they significantly increase the predicted rate of type Ibc supernovae (SNe) relative to type II SNe to the level observed in the 11HUGS galaxies. We also find that instead of assuming a constant star formation history (SFH) for the galaxies our best fitting models have a star formation rate (SFR) that peaked more than 3 Myrs ago.