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Based upon the kinematics of ten globular clusters, it has recently beenclaimed that the ultra-diffuse galaxy, NCD 1052-DF2, lacks a significantquantity of dark matter. Dynamical analyses have generally assumed that thisgalaxy is pressure supported, with the relatively small velocity dispersion ofthe globular cluster population indicating the deficit of dark matter. However,the presence of a significant rotation of the globular cluster population couldsubstantially modify this conclusion. Here we present the discovery of such asignature of rotation in the kinematics of NGC 1052-DF2's globular clusters,with a velocity amplitude of $\sim12.44^{+4.40}_{-5.16}$ km/s, which, throughBayesian model comparison, represents a marginally better fit to the availablekinematic data; note that this rotation is distinct from, and approximatelyperpendicular to, the recently identified rotation of the stellar component ofNGC 1052-DF2. Assuming this truly represents an underlying rotation, it isshown that the determined mass depends upon the inclination of the rotationalcomponent and, with a moderate inclination, the resultant mass to light ratiocan exceed $M/L\sim10$.

The Globular Cluster Population of NGC 1052-DF2: Evidence for Rotation