On the evolution of structural parameters of old globular clusters in
  the Large Magellanic Cloud
  We present result from DECam SDSS i PSF photometry of the radial stellar
density profiles of the Large Magellanic Cloud (LMC) old globular clusters
(GCs) NGC1841, 2210, Hodge11 and Reticulum, which extent out of ~ 380 pc from
their centres. We found that the studied LMC GCs would not seem to exhibit
extended stellar structures like those frequently seen in Galactic globular
clusters (GGCs), which could suggest that the LMC gravitational field has not
been efficient in stripping stars off its GCs. The concentration parameter $c$
of the studied LMC GCs would seem to depend on both the internal dynamics and
the position of the GC in the galaxy, as the Jacobi-to-cluster radius ratio
does. When comparing them with GGCs with similar masses and age-to-half-mass
relaxation times ratios, the studied LMC GCs would seem to have the smallest
concentration parameter $c$ values and step aside of the GGC relationship in
the core-to-half-light radius ratio ($r_c/r_h$) vs half-light-to-tidal radius
ratio ($r_h/r_t$) plane. These observational differences could suggest that
other conditions, like the gravitational potential of the host galaxy and/or
the orbital parameters (e.g. halo- or disc- like orbits), could play some role
in the evolution of the structural parameters of these two GC populations.
