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Globular clusters (GCs) are typically old, with most having formed at z >~ 2.This makes understanding their birth environments difficult, as they aretypically too distant to observe with sufficient angular resolution to resolveGC birth sites. Using 25 cosmological zoom-in simulations of Milky Way-likegalaxies from the E-MOSAICS project, with physically-motivated models for starformation, feedback, and the formation, evolution, and disruption of GCs, weidentify the birth environments of present-day GCs. We find roughly half of GCsin these galaxies formed in-situ (52.0 +/- 1.0 per cent) between z ~ 2 - 4, inturbulent, high-pressure discs fed by gas that was accreted without ever beingstrongly heated through a virial shock or feedback. A minority of GCs formduring mergers (12.6 +/- 0.6 per cent in major mergers, and 7.2 +/- 0.5 percent in minor mergers), but we find that mergers are important for preservingthe GCs seen today by ejecting them from their natal, high density interstellarmedium (ISM), where proto-GCs are rapidly destroyed due to tidal shocks fromISM substructure. This chaotic history of hierarchical galaxy assembly acts tomix the spatial and kinematic distribution of GCs formed through differentchannels, making it difficult to use observable GC properties to distinguishGCs formed in mergers from ones formed by smooth accretion, and similarly GCsformed in-situ from those formed ex-situ. These results suggest a simplepicture of GC formation, in which GCs are a natural outcome of normal starformation in the typical, gas-rich galaxies that are the progenitors ofpresent-day galaxies.

Where did the globular clusters of the Milky Way form? Insights from the E-MOSAICS simulations