Supernova progenitors and iron density evolution from SN rate evolution measurements

TL;DR

This paper analyzes supernova rate data to understand their progenitors, star formation history, and iron density evolution, finding limited constraints from cosmic SNIa rates but more insights from galaxy clusters.

Contribution

It provides new estimates of iron density evolution and assesses the progenitor models of supernovae using extensive supernova rate data.

Findings

Cosmic SNIa rate has limited power to constrain progenitor models.

SNe rates are compatible with a Salpeter IMF and progenitor mass > 10 Msun.

Estimated local iron abundance from SNe is about 0.1 solar.

Abstract

Using an extensive compilation of literature supernova rate data we study to which extent its evolution constrains the star formation history, the distribution of the type Ia supernova (SNIa) progenitor's lifetime, the mass range of core-collapse supernova (CCSN) progenitors, and the evolution of the iron density in the field. We find that the diagnostic power of the cosmic SNIa rate on their progenitor model is relatively weak. More promising is the use of the evolution of the SNIa rate in galaxy clusters. We find that the CCSN rate is compatible with a Salpeter IMF, with a minimum mass for their progenitors > 10 Msun. We estimate the evolution in the field of the iron density released by SNe and find that in the local universe the iron abundance should be ~ 0.1 solar. We discuss the difference between this value and the iron abundance in clusters.