text: 272,182,1453727027723341825,726837554000084993,Jeremy Bailin,"Paper day! We've studied the effect of supernova self-enrichment in globular clusters (GCs) to figure out what the Milky Way's GCs looked like when they formed based on their current metallicity and iron abundance spread and/or mass. 1/3 <LINK> Self enrichment (a) makes GCs more metal-rich than the gas they originally formed from, and (b) introduces star-to-star variation in iron abundance. We can measure (b) and use it to correct for (a)! The correction is usually small, but can be up to 0.5 dex. 2/3 <LINK> This allows us to get a more accurate view of how individual pieces of the Milky Way enriched themselves with heavy elements over time. ""We"" = me + excellent undergrad researcher Ryker von Klar. Keep an eye out for his grad school apps next year! 3/3 <LINK>",https://arxiv.org/abs/2110.14571,"Intrinsic iron abundance spreads in globular clusters, although usually small, are very common, and are signatures of self enrichment: some stars within the cluster have been enriched by supernova ejecta from other stars within the same cluster. We use the Bailin (2018) self enrichment model to predict the relationship between properties of the protocluster -- its mass and the metallicity of the protocluster gas cloud -- and the final observable properties today -- its current metallicity and the internal iron abundance spread. We apply this model to an updated catalog of Milky Way globular clusters where the initial mass and/or the iron abundance spread is known to reconstruct their initial metallicities. We find that with the exception of the known anomalous bulge cluster Terzan 5 and three clusters strongly suspected to be nuclear star clusters from stripped dwarf galaxies, the model provides a good lens for understanding their iron spreads and initial metallicities. We then use these initial metallicities to construct age-metallicity relations for kinematically-identified major accretion events in the Milky Way's history. We find that using the initial metallicity instead of the current metallicity does not alter the overall picture of the Milky Way's history, since the difference is usually small, but does provide information that can help distinguish which accretion event some individual globular clusters with ambiguous kinematics should be associated with, and points to potential complexity within the accretion events themselves. ","Globular Cluster Intrinsic Iron Abundance Spreads: II. Protocluster