only marginally consistent with a Magellanic origin.

More stringent constraints may be obtained by combining the results from Fig. \[fig:aitoff\] and Fig. \[fig:r\_vr\], since membership to the LMC group is only likely for systems in narrow regions of the four dimensional space drawn by (i) position on the sky $(l,b)$; (ii) radial velocity $V_r$, and (iii) Galactocentric distance $r_{GC}$. We illustrate this in Fig. \[fig:r\_vr\_each\_wv\], where we plot the distance and radial velocity of all LMCa particles whose positions on the sky fall within $5^\circ$ of each individual dwarf.

The top two panels on the left of Fig. \[fig:r\_vr\_each\_wv\] are meant to illustrate the analysis procedure. For the case of the LMC (top left) most particles in the LMCa subhalo are, by construction (Sec. \[SecLMCaCoord\]), at the observed location and radial velocity of the LMC (shown with a blue square). The SMC panel illustrates that most LMCa particles selected in that direction of the sky ($b=-44.3^\circ$, $l=302.8^\circ$) are at $\sim 58$ kpc from the Galactic center and have, on average, a radial velocity of $\sim 5$ km/s, which is in excellent agreement with the observed SMC values (blue square).

The red vertical bands in the panels of Fig. \[fig:r\_vr\_each\_wv\] indicate 