data are shown in the bottom two rows of Fig. \[fig:r\_vr\_each\_wv\]. From this comparison we conclude that Dra 2 has little chance of LMC association. Likewise, Ret 2, Tuc 2 and Gru 1 have velocities only marginally consistent with a Magellanic relation. Hy II, on the other hand, has the correct radial velocity for its distance, despite its large angular separation from the LMC, at the far northern edge region of the leading stream. The only clear candidate for Magellanic association is Hor 1, which is well within the expected velocity-distance range at its location.

![Galactocentric distance vs. radial velocity for LMCa particles within $5^\circ$ from each observed dwarf (blue squares), as labeled. Particles with $r_{GC}$ within $20\%$ of the observed distance fall within the red shaded area, and are used to “predict” the radial velocity expected for LMC association (see black velocity histograms on the right of each panel). The top three panels are meant to illustrate the procedure for well studied systems. The LMC sits at the middle of the distribution [*by construction*]{}. The SMC is a likely LMC satellite; Fornax is not. The bottom two rows show the newly discovered dwarfs for which kinematic measurements are available. 