with black squares; new dwarfs with measured kinematics are shown with black starred symbols. The little overlap between Fornax, Gru 1 and Tuc 2 and the LMCa debris implies a low probability of prior association between these dwarfs and the LMC, assuming first infall. Hor 1 is the dwarf most likely to have had a Magellanic association. []{data-label="fig:r_vr"}](figs/r_vr_newdwarfs_v5_snp0403.pdf "fig:"){width="100mm"}\

The distance gradients with Galactic latitude shown in Figs. \[fig:aitoff\] and  \[fig:aitoff\_box\] result from the fact that LMCa is close to pericenter and, therefore, at roughly the minimum distance of all associated debris. Debris north of the LMC is farther away and moving out (already past pericenter), whereas debris to the south is also farther away but moving in (has yet to reach pericenter). This induces a correlated signature in the radial velocities, which we explore next.

LMCa debris: radial velocities {#SecLMCaRV}
------------------------------

We explore the correlation between radial velocity and Galactic latitude in Fig. \[fig:r\_vr\]. This figure shows the Galactocentric radial velocity $V_r$ as a function of distance $r_{GC}$ for LMCa debris in the Galactic longitude range $l=[210^\circ$$-$$360^\circ]$, which encloses the stream and the positions of the DES dwarfs.

Particles are colored according to their Galactic latitude, in the range 