2022/10/04 by James W. Johnson, C. S. Kochanek, Johnson, James W. +3 · 1 citation
Physics and Astronomy · #Gamma-ray bursts and supernovae
paper · pdf · doi:10.48550/arxiv.2210.01818
The scaling of the specific Type Ia supernova (SN Ia) rate with host galaxy stellar mass NIa / M_⋆ ∼ M_⋆-0.3 as measured in ASAS-SN and DES strongly suggests that the number of SNe Ia produced by a stellar population depends inversely on its metallicity. We estimate the strength of the required metallicity dependence by combining the average star formation histories (SFHs) of galaxies as a function of their stellar mass with the mass-metallicity relation (MZR) for galaxies and common parametrizations for the SN Ia delay-time distribution. The differences in SFHs can account for only ∼30% of the increase in the specific SN Ia rate between stellar masses of M_⋆ = 1010 and 107.2 M_\odot. We find that an additional metallicity dependence of approximately ∼Z-0.5 is required to explain the observed scaling. This scaling matches the metallicity dependence of the close binary fraction observed in APOGEE, suggesting that the enhanced SN Ia rate in low-mass galaxies can be explained by a combination of their more extended SFHs and a higher binary fraction due to their lower metallicities. Due to the shape of the MZR, only galaxies below M_⋆ ≈ 3×109 M_\odot are significantly affected by the metallicity-dependent SN Ia rates. The NIa / M_⋆ ∼ M_⋆-0.3 scaling becomes shallower with increasing redshift, dropping by factor of ∼2 at 107.2 M_\odot between z = 0 and 1 with our ∼Z-0.5 scaling. With metallicity-independent rates, this decrease is a factor of ∼3. We discuss the implications of metallicity-dependent SN Ia rates for one-zone models of galactic chemical evolution.