other globular cluster systems (e.g., the Na-O anti-correlation; @carretta2009). Therefore, other than its physical association with the Sgr remnant, M54 does not stand out from other GCs in terms of its chemical abundance patterns, similar to the metal-poor GCs Terzan 8 and Arp 2 (both also kinematically and spatial associated with the Sgr stream @b88). On the other hand, Hodge 11 in the LMC at \[Fe/H\] = -2.0 does have lower \[$\alpha$/Fe\] than MW field and GC stars[@b90]; and Ruprecht 106 has an anomalously low \[$\alpha$/Fe\] ratio for a MW GC [@b48].

Two metal-poor clusters that have been associated with the Sgr stream are NGC5024 (M53) and NGC5466 [@b50; @b51]. Both of these clusters are more metal-poor than M54 (each at \[Fe/H\] $\sim -2$, Harris 1996), which means that detailed chemistry could be inconclusive as to their origins in the Sgr dwarf galaxy. We have opted to study the chemistry in these GCs regardless though because (1) there are few published chemistries for these clusters and (2) they are both associated with other interesting dynamical structures. NGC5466 has a large tidal tail [@b55] it appears to have no association with the Sgr stream, and knowing the chemistry of this GC 