Formation histories of stars, clusters, and globular clusters in the E-MOSAICS simulations

The formation histories of globular clusters (GCs) are a key diagnostic for understanding their relation to the evolution of the Universe through COSMiC time. We use the suite of 25 cosmological ZOOM-irl simulations of present-day Milky Way-mass galaxies from the E. MOSAICS project to study the formation histories of stars, clusters, and GCs, and how these are affected by the environmental dependence of the cluster formation physics. We rind that the median lookback time of GC formation in these galaxies is-10.73 Gyr (z = 2.1), roughly 2.5 Gyr earlier than that of the field stars (-8.34 Gyr or z = 1.1). The epoch of peak GC formation is mainly determined by the time evolution of the maximum cluster mass, which depends on the galactic environment and largely increases with the gas pressure. Different metallicity subpopulations of stars, clusters, and GCs present overlapping formation histories, implying that star and cluster formation represent continuous processes. The metal-poor GCs (-2.5 9 [Fe/II] 9-1.5) of our galaxies are older than the metal-rich GC subpopulation (-1.0 9 [Fe/II] 9-0.5), forming 12.13 Gyr and 10.15 Gyr ago (z = 3.7 and z = 1.8), respectively. The median ages of GCs are found to decrease gradually with increasing metallicity, which suggests different GC metallicity subpopulations do not form independently and their spatial and kinematic distributions are the result of their evolution in the context of hierarchical galaxy formation and evolution. We predict that proto-GC formation is most prevalent at 2 < z < 3, which could be tested with observations of lensed galaxies using MST+