Footprints in the sand: What can globular clusters tell us about NGC
  4753 past?
  NGC 4753 is a bright (M_V approx -22.3) lenticular galaxy. It is a very
interesting target to test different theories of formation of lenticular
galaxies, due to its low-density environment and complex structure. We perform
the first comprehensive study of NGC 4753 globular cluster system (GCS), using
Gemini/GMOS and CTIO/MosaicII images. Our results indicate a rather poor GCS of
approx 1000 members. Its azimuthal distribution follows the shape of the galaxy
bulge. The GC colour distribution is peculiar, presenting an intermediate
subpopulation in addition to blue and red ones. This intermediate subgroup can
be explained by a single stellar population with an age of 1.5-3 Gyr and 0.5-1
Z_o. The GC specific frequency S_N = 1.3+/-0.15 is surprisingly low for a
galaxy of its class. The GC luminosity function (GCLF) is also peculiar, with
an excess of bright GCs compared to the expected gaussian distribution. The
underlying galaxy body has significant substructure, with remnants of spiral
arms, dust filaments, and isophote twisting. This, and the fact that NGC 4753
hosted two type Ia SNe, support the possibility that the intermediate GC
subpopulation may have originated during a recent merger, 1-3 Gyr ago.
