Abstract

The assembly history of the Milky Way (MW) is a rapidly evolving subject, with numerous small accretion events and at least one major merger proposed in the MW’s history. Accreted alongside these dwarf galaxies are globular clusters (GCs), which act as spatially coherent remnants of these past events. Numerous studies have explored the dynamical connection between accreted MW G Cs and their progenitors, tagging GCs to specific merger events in energy, z-angular momentum space (Myeong 2018, Myeong 2019, Massari 2019). But as of yet, no strong chemical “tag” has been found to support the dynamical associations (Horta 2020). This begs the question, does such a tag exist? If so, the relatively small range of metallicity found within GCs, coupled with high resolution chemical abundances, could serve as a sharp probe of the chemical evolution history of their host galaxies. In this talk, I will present results from a high precision differential analysis study of the proposed GC siblings, NGC 362 and NGC 288 discussing the chemodynamical evidence for and against siblinghood and support for the ratio of [Eu/Mg] as a chemical link between NGC 362 and Gaia-Enceladus-Sausage. Finally, I will present initial results from a differential abundance study of the GC M54 and the Sagittarius dwarf galaxy, highlighting how the only intact GC-progenitor system could set the scale for how similar GCs and their hosts truly are.