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Intrinsic iron abundance spreads in globular clusters, although usuallysmall, are very common, and are signatures of self enrichment: some starswithin the cluster have been enriched by supernova ejecta from other starswithin the same cluster. We use the Bailin (2018) self enrichment model topredict the relationship between properties of the protocluster -- its mass andthe metallicity of the protocluster gas cloud -- and the final observableproperties today -- its current metallicity and the internal iron abundancespread. We apply this model to an updated catalog of Milky Way globularclusters where the initial mass and/or the iron abundance spread is known toreconstruct their initial metallicities. We find that with the exception of theknown anomalous bulge cluster Terzan 5 and three clusters strongly suspected tobe nuclear star clusters from stripped dwarf galaxies, the model provides agood lens for understanding their iron spreads and initial metallicities. Wethen use these initial metallicities to construct age-metallicity relations forkinematically-identified major accretion events in the Milky Way's history. Wefind that using the initial metallicity instead of the current metallicity doesnot alter the overall picture of the Milky Way's history, since the differenceis usually small, but does provide information that can help distinguish whichaccretion event some individual globular clusters with ambiguous kinematicsshould be associated with, and points to potential complexity within theaccretion events themselves.

Globular Cluster Intrinsic Iron Abundance Spreads: II. Protocluster Metallicities and the Age-Metallicity Relations of Milky Way Progenitors