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We investigate aluminum abundance variations in the stellar populations ofglobular clusters using both literature measurements of sodium and aluminum andAPOGEE measurements of nitrogen and aluminum abundances. For the latter, weshow that the Payne is the most suitable of the five available abundancepipelines for our purposes. Our combined sample of 42 globular clusters spansapproximately 2 dex in [Fe/H] and 1.5 dex in $\log{M_{GC}/M_{\odot}}$. We findno fewer than five globular clusters with significant internal variations innitrogen and/or sodium with little-to-no corresponding variation in aluminum,and that the minimum present-day cluster mass for aluminum enrichment inmetal-rich systems is $\log{M_{GC}/M_{\odot}} \approx 4.50 +2.17(\rm{[Fe/H]}+1.30)$. We demonstrate that the slopes of the [Al/Fe] vs[Na/Fe] and [Al/Fe] vs [N/Fe] relations for stars without field-like abundancesare approximately log-linearly dependent on both the metallicity and thestellar mass of the globular clusters. In contrast, the relationship between[Na/Fe] and [N/Fe] shows no evidence of such dependencies. This suggests thatthere were (at least) two classes of non-supernovae chemical polluters thatwere common in the early universe, and that their relative contributions withinglobular clusters somehow scaled with the metallicity and mass of globularclusters. The first of these classes is predominantly responsible for the CNOand NeNa abundance variations, and likewise the second for the MgAl abundancevariations. 47 Tuc and M4 are particularly striking examples of this dichotomy.As an auxiliary finding, we argue that abundance variations among Terzan 5stars are consistent with it being a normal globular cluster.

The Relationship Between Globular Cluster Mass, Metallicity, and Light Element Abundance Variations