Abstract

Globular clusters (GCs) are among the most ancient objects in the local Universe, acting as tracers of galaxy formation across both space and time. With the recent JWST discovery of nitrogen-rich star formation in a redshift 11 galaxy, and the discovery that over 50% of the in-situ stars in the Milky Way (MW) likely formed in clusters, understanding the role of GCs in the context of galaxy evolution is becoming ever more important. The MW hosts a large (~150) and diverse population of GCs. Among these clusters, a fraction are thought to have formed in-situ, alongside the MW, while others were likely accreted alongside disrupted dwarf galaxies. A small number of MW G Cs may themselves be the sole remaining remnants of disrupted dwarf galaxies as stripped nuclear star clusters. In this talk I will discuss ongoing work to identify the origins of accreted GCs, highlighting the strength of combining high resolution chemical abundances with dedicated dynamical simulations. I will present results for populations of accreted GCs as well as individuals, presenting initial results as to the origins of the MW’s two most enigmatic GCs, NGC 2419 and M 22 .