Only Hy II and Hor 1 show velocities consistent with those expected for prior association with the LMC. []{data-label="fig:r_vr_each_wv"}](figs/r_vr_closesky_v9_withvel_snp0403.pdf){width="84mm"}

![Same as Fig. \[fig:r\_vr\_each\_wv\] but for the new dwarfs with no measured $V_r$. The Galactocentric distances for Pic 1, Eri 2 and Tuc 3 seem inconsistent with the distances measured for the LMCa debris around their positions on the sky. On the other hand, Ret 3, Hor 2 and several of the Tucanas show high chance of association, at least based on their positions and distances alone.[]{data-label="fig:r_vr_each_nov"}](figs/r_vr_closesky_v9_withoutvel_snp0403.pdf){width="0.89\linewidth"}

Predicted radial velocities for candidate Magellanic satellites {#SecMagSatRV}
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We can use the procedure described in the previous subsection to predict the radial velocities that the remaining “new dwarfs” would have if they were truly Magellanic satellites. We show this in Fig. \[fig:r\_vr\_each\_nov\], which lists dwarfs in order of decreasing Galactic latitude. Inspection of individual panels suggests some preliminary conclusions. The Galactocentric distances measured for Pic 1 and Eri 2 seem inconsistent with previous association with the LMC. Cra 2 is in the same category, given the very little overlap with the edge of the leading arm of the stream. Aside from those three cases, all other dwarfs show some degree of overlap in 