Trading oxygen for iron I: the [O/Fe] -- specific star formation rate relation of galaxies

TL;DR

This paper investigates the [O/Fe] ratio's relation to specific star formation rate in galaxies, combining simulations, theoretical models, and observational data to understand chemical evolution and feedback processes.

Contribution

It introduces the [O/Fe]-sSFR relation as a tool to infer iron abundance from oxygen measurements, supported by empirical data and theoretical consistency.

Findings

[O/Fe] decreases with lower sSFR in galaxies.

The relation aligns with Milky Way stellar data.

The relation's universality aids in chemical abundance studies.

Abstract

Our current knowledge of star-forming metallicity relies primarily on gas-phase oxygen abundance measurements. This may not allow one to accurately describe differences in stellar evolution and feedback driven by variations in iron abundance. $\alpha$-elements (such as oxygen) and iron are produced by sources that operate on different timescales and the link between them is not straightforward. We explore the origin of the [O/Fe] - specific SFR (sSFR) relation, linking chemical abundances to galaxy formation timescales. This relation is followed by star-forming galaxies across redshifts according to cosmological simulations and basic theoretical expectations. Its apparent universality makes it suitable for trading the readily available oxygen for iron abundance. The relation is determined by the relative iron production efficiency of core-collapse and type Ia supernovae and the delay time distribution of the latter -- uncertain factors that could be constrained empirically with the [O/Fe]-sSFR relation. We compile and homogenise a literature sample of star-forming galaxies with observational iron abundance determinations to place first constraints on the [O/Fe]-sSFR relation over a wide range of sSFR. The relation shows a clear evolution towards lower [O/Fe] with decreasing sSFR and a flattening above log(sSFR/yr)>-9. The result is broadly consistent with expectations, but better constraints are needed to inform the models. We independently derive the relation from old Milky Way stars and find a remarkable agreement between the two, as long as the recombination-line absolute oxygen abundance scale is used in conjunction with stellar metallicity measurements.