Galactic Chemical Evolution Models Favor an Extended Type Ia Supernova Delay-time Distribution

• Published in: The Astrophysical journal Vol. 973; no. 1; pp. 55 - 80
• Main Authors: Dubay, Liam O., Johnson, Jennifer A., Johnson, James W.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01-09-2024; IOP Publishing
• Subjects: Abundance; Astronomical models; Chemical abundances; Chemical enrichment; Chemical evolution; Chronology; Galactic evolution; Galaxy chemical evolution; Goodness of fit; Interstellar chemistry; Interstellar matter; Interstellar medium; Milky Way; Milky Way disk; Milky Way evolution; Skewed distributions; Star & galaxy formation; Star formation; Stars; Stellar age; Stellar evolution; Supernova; Supernovae; the Milky Way
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad61df

Abstract Type Ia supernovae (SNe Ia) produce most of the Fe-peak elements in the Universe and therefore are a crucial ingredient in galactic chemical evolution models. SNe Ia do not explode immediately after star formation, and the delay-time distribution (DTD) has not been definitively determined by supernova surveys or theoretical models. Because the DTD also affects the relationship among age, [Fe/H], and [ α /Fe] in chemical evolution models, comparison with observations of stars in the Milky Way is an important consistency check for any proposed DTD. We implement several popular forms of the DTD in combination with multiple star formation histories for the Milky Way in multizone chemical evolution models that include radial stellar migration. We compare our predicted interstellar medium abundance tracks, stellar abundance distributions, and stellar age distributions to the final data release of the Apache Point Observatory Galactic Evolution Experiment. We find that the DTD has the largest effect on the [ α /Fe] distribution: a DTD with more prompt SNe Ia produces a stellar abundance distribution that is skewed toward a lower [ α /Fe] ratio. While the DTD alone cannot explain the observed bimodality in the [ α /Fe] distribution, in combination with an appropriate star formation history it affects the goodness of fit between the predicted and observed high- α sequence. Our model results favor an extended DTD with fewer prompt SNe Ia than the fiducial t −1 power law.