more detail the position of individual dwarfs as well as the distance gradient expected for this section of the stream. This figure also shows that Col 1 lies outside of the LMCa debris footprint. This, combined with its large distance ($\sim 182$ kpc) makes a Magellanic association rather unlikely [see also @Drlica2015]. We therefore exclude Col 1 from the rest of our analysis, together with Sag 2, whose position in the sky is not favorable either. Furthermore, we also remove Indus 1 from our analysis since it has now been classified as a stellar cluster rather than a dwarf galaxy [@Kim2015c].

![Galactocentric distance $r_{GC}$ vs. radial velocity $V_r$ for LMCa particles at first pericenter, color-coded by Galactic latitude $b$ ($-80^\circ<b<0^\circ$; see color bar on right). For clarity, we only show the Galactic longitude range $l=[210^\circ,360^\circ]$, which encompasses most of the LMCa material in Fig. \[fig:aitoff\]. Note the correlation between latitude and radial velocity, with the leading arm having already passed through pericenter (positive $V_r$) and the trailing material still approaching the Galaxy with $V_r < 0$. As before, the LMC and SMC are shown with grey squares and other previously known dwarfs in this region of the sky are marked 