Evidence of differential tidal effects in the old globular cluster
  population of the Large Magellanic Cloud
  We present for the first time extended stellar density and/or surface
brightness radial profiles for almost all the known Large Magellanic Cloud
(LMC) old globular clusters (GCs). These were built from DECam images and reach
out to ~ 4 times the GCs' tidal radii. The background subtracted radial
profiles reveal that the GCs located closer than ~ 5 kpc from the LMC centre
contain an excess of stars in their outermost regions with respect to the
stellar density expected from a King profile. Such a residual amount of stars -
not seen in GCs located farther than ~ 5 kpc from the LMC centre-, as well as
the GCs' dimensions, show a clear dependence with the GCs' positions in the
galaxy, in the sense that, the farther the GC from the centre of the LMC, the
larger both the excess of stars in its outskirts and size. Although the masses
of GCs located inside and outside ~ 5 kpc are commensurate, the outermost
regions of GCs located closer than ~ 5 kpc from the LMC centre appear to have
dynamically evolved more quickly. These outcomes can be fully interpreted in
the light of the known GC radial velocity disc-like kinematics, from which GCs
have been somehow mostly experiencing the influence of the LMC gravitational
field at their respective mean distances from the LMC centre.
