a (generous) $20\%$ uncertainty in the distance estimate to each dwarf; its intersection with LMCa particles is used to draw the velocity histograms in the right-hand side of each panel. Coincidence between the velocity of the blue square and the histogram indicates that the observed velocity is not unexpected in a scenario where the dwarf originates from a disrupted LMC group. The velocity histograms may therefore be used to “predict” the radial velocity of dwarfs for which kinematic data is not yet available, [*assuming*]{} a Magellanic origin.

As may be seen from Fig. \[fig:r\_vr\_each\_wv\], and not surprisingly, the SMC passes these tests handily, making its association with the LMC quite likely. On the other hand, the probability of association of a dwarf like Fornax is quite remote. Most debris in that direction of the sky are at much closer distances, and the little that overlaps in distance with Fornax (two particles) has a rather high positive radial velocity, quite unlike that observed. This illustrates the arguments used by S11 to exclude an LMC association not only for Fornax but also for all other Galactic satellites known at that time in case of first infall.

The $6$ “new dwarfs” with kinematic 