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We study the present-day rotational velocity ($V_{rot}$) and velocitydispersion (${\sigma}$) profiles of the globular cluster (GC) systems in asample of 50 lenticular (S0) galaxies from the E-MOSAICS galaxy formationsimulations. We find that 82% of the galaxies have GCs that are rotating alongthe photometric major axis of the galaxy ($aligned$), while the remaining 18%of the galaxies do not ($misaligned$). This is generally consistent with theobservations from the SLUGGS survey. For the $aligned$ galaxies, classified as$peaked$ $and$ $outwardly$ $decreasing$ (49%), $flat$ (24%) and $increasing$(27%) based on the $V_{rot}/{\sigma}$ profiles out to large radii, we do notfind any clear correlation between these present-day $V_{rot}/{\sigma}$profiles of the GCs and the past merger histories of the S0 galaxies, unlike inprevious simulations of galaxy stars. For just over half of the $misaligned$galaxies, we find that the GC misalignment is the result of a major mergerwithin the last 10 Gyr so that the $ex$-$situ$ GCs are misaligned by an anglebetween 0{\deg} (co-rotation) to 180{\deg} (counter-rotation) with respect tothe $in$-$situ$ GCs, depending on the orbital configuration of the merginggalaxies. For the remaining $misaligned$ galaxies, we suggest that the$in$-$situ$ metal-poor GCs, formed at early times, have undergone more frequentkinematic perturbations than the $in$-$situ$ metal-rich GCs. We also find thatthe GCs accreted early and the $in$-$situ$ GCs are predominantly located within0.2 virial radii ($R_{200}$) from the centre of galaxies in 3D phase-spacediagrams.

The present-day globular cluster kinematics of lenticular galaxies from the E-MOSAICS simulations and their relation to the galaxy assembly histories