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Massive early-type galaxies typically have two subpopulations of globularclusters (GCs) which often reveal radial colour (metallicity) gradients.Collating gradients from the literature, we show that the gradients in themetal-rich and metal-poor GC subpopulations are the same, within measurementuncertainties, in a given galaxy. Furthermore, these GC gradients are similarin strength to the {\it stellar} metallicity gradient of the host galaxy. Atthe very largest radii (e.g. greater than 8 galaxy effective radii) there issome evidence that the GC gradients become flat with near constant meanmetallicity. Using stellar metallicity gradients as a proxy, we probe theassembly histories of massive early-type galaxies with hydrodynamicalsimulations from the Magneticum suite of models. In particular, we measure thestellar metallicity gradient for the in-situ and accreted components over asimilar radial range as those observed for GC subpopulations. We find that thein-situ and accreted stellar metallicity gradients are similar but have alarger scatter than the metal-rich and metal-poor GC subpopulations gradientsin a given galaxy. We conclude that although metal-rich GCs are predominatelyformed during the in-situ phase and metal-poor GCs during the accretion phaseof massive galaxy formation, they do not have a strict one-to-one connection.

Metallicity gradients in the globular cluster systems of early-type galaxies: In-situ and accreted components?