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Stellar halos and globular cluster (GC) systems contain valuable informationregarding the assembly history of their host galaxies. Motivated by thedetection of a significant rotation signal in the outer halo GC system of M31,we investigate the likelihood of detecting such a rotation signal inprojection, using cosmological simulations. To this end we select subsets oftagged particles in the halos of the Aquarius simulations to represent mock GCsystems, and analyse their kinematics. We find that GC systems can exhibit anon-negligible rotation signal provided the associated stellar halo also has anet angular momentum. The ability to detect this rotation signal is highlydependent on the viewing perspective, and the probability of seeing a signallarger than that measured in M31 ranges from 10% to 90% for the different halosin the Aquarius suite. High values are found from a perspective such that theprojected angular momentum of the GC system is within 40 deg of the rotationaxis determined via the projected positions and line-of-sight velocities of theGCs. Furthermore, the true 3D angular momentum of the outer stellar halo isrelatively well aligned, within 35 deg, with that of the mock GC systems. Weargue that the net angular momentum in the mock GC systems arises naturallywhen the majority of the material is accreted from a preferred direction,namely along the dominant dark matter filament of the large-scale structurethat the halos are embedded in. This, together with the favourable edge-on viewof M31's disk suggests that it is not a coincidence that a large rotationsignal has been measured for its outer halo GC system.

The kinematics of globular clusters systems in the outer halos of the Aquarius simulations