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Stellar population studies of globular clusters have suggested that thebrightest clusters in the Galaxy might actually be the remnant nuclei of dwarfspheroidal galaxies. If the present Galactic globular clusters formed withinlarger stellar systems, they are likely surrounded by extra-tidal halos and/ortails made up of stars that were tidally stripped from their parent systems.The stellar surroundings around globular clusters are therefore one of the bestplaces to look for the remnants of an ancient dwarf galaxy. Here an attempt ismade to search for tidal debris around the supernovae enriched globularclusters M22 and NGC 1851 as well as the kinematically unique cluster NGC 3201.The stellar parameters from the Radial Velocity Experiment (RAVE) are used toidentify stars with RAVE metallicities, radial velocities andelemental-abundances consistent with the abundance patterns and properties ofthe stars in M22, NGC 1851 and NGC 3201. The discovery of RAVE stars that maybe associated with M22 and NGC 1851 are reported, some of which are atprojected distances of ~10 degrees away from the core of these clusters.Numerous RAVE stars associated with NGC 3201 suggest that either the tidalradius of this cluster is underestimated, or that there are some unbound starsextending a few arc minutes from the edge of the cluster's radius. No furtherextra-tidal stars associated with NGC 3201 could be identified. The brightmagnitudes of the RAVE stars make them easy targets for high resolutionfollow-up observations, allowing an eventual further chemical tagging tosolidify (or exclude) stars outside the tidal radius of the cluster as tidaldebris. In both our radial velocity histograms of the regions surrounding NGC1851 and NGC 3201, a peak of stars at 230 km/s is seen, consistent withextended tidal debris from omega Centauri.

Spectroscopic Signatures of Extra-Tidal Stars Around the Globular Clusters NGC 6656 (M22), NGC 3201 and NGC 1851 from RAVE