$-80^\circ<b<0^\circ$ (see color bar). Fig. \[fig:r\_vr\] shows a clear gradient in radial velocity with Galactic latitude, showing generally positive values (outward moving) for particles north of the position of the LMC (i.e., $b_{\rm LMC} > -32.9^\circ$) and negative values (infalling) for those south of that. Although the latitude trend is clear, the dispersion about the mean trend is quite large. This is because the velocity dispersion of LMCa before infall was quite substantial (at $z_{\rm id}=0.9$, $\sigma_{200}=V_{200}/\sqrt 2=44.5$ km/s), making the tidally-induced stream quite thick. As a result, the constraints on a possible Magellanic origin provided by $b$, $r_{\rm GC}$ and $V_r$ alone are relatively lax, and serve mainly to rule out the most unlikely candidates.

For example, Fig. \[fig:r\_vr\] shows that Fornax (even though it is close to the stream in sky projection) has a distance that is too large to be associated with the LMC, whereas the SMC, as expected, lies well within the velocity-distance range spanned by the LMCa debris. Starred symbols show the “new dwarfs” that fall in this region of the sky and for which kinematic measurements are available [@Walker2016; @Koposov2015b]: Hor 1, Ret 2 are clear candidates, whereas Tuc 2 and Gru 1 seem 