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Globular clusters (GCs) have been posited, alongside dwarf galaxies, assignificant contributors to the field stellar population of the Galactic halo.In order to quantify their contribution, we examine the fraction of halo starsformed in stellar clusters in the suite of 25 present-day Milky Way-masscosmological zoom simulations from the E-MOSAICS project. We find that a medianof $2.3$ and $0.3$ per cent of the mass in halo field stars formed in clustersand GCs, defined as clusters more massive than $5\times 10^3$ and$10^5~M_{\odot}$, respectively, with the $25$-$75$th percentiles spanning$1.9$-$3.0$ and $0.2$-$0.5$ per cent being caused by differences in theassembly histories of the host galaxies. Under the extreme assumption that nostellar cluster survives to the present day, the mass fractions increase to amedian of $5.9$ and $1.8$ per cent. These small fractions indicate that thedisruption of GCs plays a sub-dominant role in the build-up of the stellarhalo. We also determine the contributed halo mass fraction that would presentsignatures of light-element abundance variations considered to be unique toGCs, and find that clusters and GCs would contribute a median of $1.1$ and$0.2$ per cent, respectively. We estimate the contributed fraction of GC starsto the Milky Way halo, based on recent surveys, and find upper limits of$2$-$5$ per cent (significantly lower than previous estimates), suggesting thatmodels other than those invoking strong mass loss are required to describe theformation of chemically enriched stellar populations in GCs.

The mass fraction of halo stars contributed by the disruption of globular clusters in the E-MOSAICS simulations