FSR 1776: a new globular cluster in the Galactic bulge?
  (ABRIDGED) Recent near-IR surveys have uncovered a plethora of new globular
cluster (GC) candidates towards the Milky Way bulge. These new candidates need
to be confirmed as real GCs and properly characterised. We investigate the
physical nature of FSR 1776. This object was originally classified as an
intermediate-age open cluster and has recently been re-discovered independently
and classified as a GC candidate (Minni 23). Firstly, we aim at confirming its
GC nature; secondly we determine its physical parameters. The confirmation of
the cluster existence is checked using the radial velocity (RV) distribution of
a MUSE data cube centred at FSR 1776. The cluster parameters are derived from
isochrone fitting to the RV-cleaned colour-magnitude diagrams (CMDs) from
visible and near-infrared photometry. The predicted RV distribution for the FSR
1776 coordinates, considering only contributions from the bulge and disc field
stars, is not enough to explain the observed MUSE RV distribution. The extra
population (12\% of the sample) is FSR 1776 with an average RV of $-103.7\pm
0.4~{\rm km}\,{\rm s}^{-1}$. The CMDs reveal that it is 10$\pm$1~Gyr old and
metal-rich, with [Fe/H]$_{phot}\approx + 0.2\pm$0.2,
[Fe/H]$_{spec}=~+0.02\pm0.01~(\sigma~=~0.14$~dex), located at the bulge
distance of 7.24$\pm$0.5~kpc with A$_{\rm V}$ $\approx$ 1.1~mag. The mean
cluster proper motions are
($\langle\mu_{\alpha}\rangle,\langle\mu_{\delta}\rangle$) $=$
($-2.3\pm1.1,-2.6\pm0.8$) ${\rm mas\, yr^{-1}}$.} FSR 1776 is an old GC located
in the Galactic bulge with a super-solar metallicity, among the highest for a
Galactic GC. This is consistent with predictions for the age-metallicity
relation of the bulge, being FSR 1776 the probable missing link between typical
GCs and the metal-rich bulge field. High-resolution spectroscopy of a larger
field of view and deeper CMDs are now required for a full characterisation.
