Radial velocity in the cluster system as a function of distance from the cluster center, expressed in core radii units, for less studied clusters. Na-rich and Na-poor stars are plotted with different symbols. The dotted line marks the tidal radius of the K66 model that best fits the surface brightness profile, according to McLaughlin & van der Marel (2005). The continuous curves are the  ± 3σ profiles of the same models, normalized to the central σ listed by Harris (1996), approximately representing the envelope of the allowed velocities for the bound members of the clusters. The dashed line marks the half-light radius, taken from Harris (1996).