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Our current knowledge of star-forming metallicity relies primarily ongas-phase oxygen abundance measurements. This may not allow one to accuratelydescribe differences in stellar evolution and feedback driven by variations iniron abundance. $\alpha$-elements (such as oxygen) and iron are produced bysources that operate on different timescales and the link between them is notstraightforward. We explore the origin of the [O/Fe] - specific SFR (sSFR)relation, linking chemical abundances to galaxy formation timescales. Thisrelation is followed by star-forming galaxies across redshifts according tocosmological simulations and basic theoretical expectations. Its apparentuniversality makes it suitable for trading the readily available oxygen foriron abundance. The relation is determined by the relative iron productionefficiency of core-collapse and type Ia supernovae and the delay timedistribution of the latter -- uncertain factors that could be constrainedempirically with the [O/Fe]-sSFR relation. We compile and homogenise aliterature sample of star-forming galaxies with observational iron abundancedeterminations to place first constraints on the [O/Fe]-sSFR relation over awide 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 isbroadly consistent with expectations, but better constraints are needed toinform the models. We independently derive the relation from old Milky Waystars and find a remarkable agreement between the two, as long as therecombination-line absolute oxygen abundance scale is used in conjunction withstellar metallicity measurements.

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