On the physical nature of globular cluster candidates in the Milky Way
  bulge
  We present results from 2MASS JKs photometry on the physical reality of
recently reported globular cluster (GC) candidates in the Milky Way (MW) bulge.
We relied our analysis on photometric membership probabilities that allowed us
to distinguish real stellar aggregates from the composite field star
population. When building colour-magnitude diagrams and stellar density maps
for stars at different membership probability levels, the genuine GC candidate
populations are clearly highlighted. We then used the tip of the red giant
branch (RGB) as distance estimator, resulting heliocentric distances that place
many of the objects in regions near of the MW bulge where no GC had been
previously recognised. Some few GC candidates resulted to be MW halo/disc
objects.Metallicities estimated from the standard RGB method are in agreement
with the values expected according to the position of the GC candidates in the
Galaxy. We finally derived from the first time their structural parameters. We
found that the studied objects have core, half-light and tidal radii in the
ranges spanned by the population of known MW GCs. Their internal dynamical
evolutionary stages will be described properly when their masses are estimated.
