Stellar density distribution along the minor axis of the Large
  Magellanic Cloud
  We studied the spatial distribution of young and old stellar populations
along the western half part of the minor axis of the Large Magellanic Cloud
(LMC) using Washington MT1 photometry of selected fields, which span a
deprojected distance range from the LMC bar centre out to ~ 31.6 kpc. We found
that both stellar populations share a mean LMC limiting radius of 8.9+-0.4 kpc;
old populations are three times more dense that young populations at that LMC
limit. When comparing this result with recent values for the LMC extension due
to north, the old populations resulted significantly more elongated than the
young ones. Bearing in mind previous claims that the elongation of the
outermost LMC regions may be due to the tidal effects of the Milky Way (MW),
our findings suggest that such a tidal interaction should not have taken place
recently. The existence of young populations in the outermost western regions
also supports previous results about ram pressure stripping effects of the LMC
gaseous disc due to the motion of the LMC in the MW halo.
