sightly all Galactocentric distances so that LMCa is, at each pericenter, at the measured distance of the LMC: $49$ kpc.

![image](figs/areasky_newdwarfs_propmotion_axisratio_v2_snp0403){width="0.89\linewidth"}\

Results {#sec:results}
=======

We first examine the sky distribution of particles associated at infall with the LMC analog subhalo (hereafter “LMCa debris”, for short). We use this footprint, as well as their radial and tangential velocities, to compare with available data for the newly-discovered dwarfs. As mentioned above, we shall interpret coincidence in sky position, radial velocity and distance between debris particles and observed dwarfs as evidence of a possible association with the LMC.

LMCa debris: sky distribution and distances {#SecLMCaSkyD}
-------------------------------------------

At the time of the first pericenter, tidal disruption due to the host halo has already set in, but most particles are still bound and close to the subhalo center. The rest of the material is distributed along a thick but well-defined tidal stream that follows the projection of the subhalo’s orbital path on the sky. A leading and trailing arm extend towards more positive and negative latitudes, respectively. The distribution of this debris roughly agrees with the position of the HI Magellanic Stream, sketched here by a line that traces the high-density HI in the sky 