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Intra-cluster (IC) populations are expected to be a natural result of thehierarchical assembly of clusters, yet their low space densities make themdifficult to detect and study. We present the first definitive kinematicdetection of an IC population of globular clusters (GCs) in the Virgo cluster,around the central galaxy, M87. This study focuses on the Virgo core for whichthe combination of NGVS photometry and follow-up spectroscopy allows us toreject foreground star contamination and explore GC kinematics over the fullVirgo dynamical range. The GC kinematics changes gradually with galactocentricdistance, decreasing in mean velocity and increasing in velocity dispersion,eventually becoming indistinguishable from the kinematics of Virgo dwarfgalaxies at $\mathrm{R>320\, kpc}$. By kinematically tagging M87 halo andintra-cluster GCs we find that 1) the M87 halo has a smaller fraction($52\pm3\%$) of blue clusters with respect to the IC counterpart ($77\pm10\%$),2) the $(g'-r')_{0}$ vs $(i'-z')_{0}$ color-color diagrams reveal a galaxypopulation that is redder than the IC population that may be due to a differentcomposition in chemical abundance and progenitor mass, and 3) the ICGCdistribution is shallower and more extended than the M87 GCs, yet stillcentrally concentrated. The ICGC specific frequency,$S_{N,\mathrm{ICL}}=10.2\pm4.8$, is consistent with what is observed for thepopulation of quenched, low-mass galaxies within 1~Mpc from the cluster'scenter. The IC population at Virgo's center is thus consistent with being anaccreted component from low-mass galaxies tidally stripped or disrupted throughinteractions, with a total mass of$\mathrm{M_{ICL,tot}=10.8\pm0.1\times10^{11}M_{\odot}}$.

The Next Generation Virgo Cluster Survey (NGVS) XXXI. The kinematics of intra-cluster globular clusters in the core of the Virgo cluster