  Physical properties were derived for the candidate open cluster La Serena 94,
recently unveiled by the VVV collaboration. Thanks to the exquisite angular
resolution provided by GeMS/GSAOI, we could characterize this system in detail,
for the first time, with deep photometry in JHK$_{s}$ - bands. Decontaminated
JHK$_{s}$ diagrams reach about 5 mag below the cluster turnoff in H. The locus
of red clump giants in the colour - colour diagram, together with an extinction
law, was used to obtain an average extinction of $A_V =14.18 \pm 0.71$. The
same stars were considered as standard - candles to derive the cluster
distance, $8.5 \pm 1.0$ kpc. Isochrones were matched to the cluster colour -
magnitude diagrams to determine its age, $\log{t(yr)}=9.12\pm 0.06$, and
metallicity, $Z=0.02\pm0.01$. A core radius of $r_{c}=0.51\pm 0.04$ pc was
found by fitting King models to the radial density profile. By adding up the
visible stellar mass to an extrapolated mass function, the cluster mass was
estimated as $M=(2.65\pm0.57) \times 10^3$ M$_{\odot}$, consistent with an
integrated magnitude of $M_{K}=-5.82\pm0.16$ and a tidal radius of
$r_{t}=17.2\pm2.1$ pc. The overall characteristics of La Serena 94 confirm that
it is an old open cluster located in the Crux spiral arm towards the fourth
Galactic quadrant and distant $7.30\pm 0.49$ kpc from the Galactic centre. The
cluster distorted structure, mass segregation and age indicate that it is a
dynamically evolved stellar system.
