Galactic open clusters ( OCs ) that survive the early gas-expulsion phase are gradually destroyed over time by the action of disruptive dynamical processes .
Their final evolutionary stages are characterized by a poorly populated concentration of stars called open cluster remnant ( OCR ) .
This study is devoted to assess the real physical nature of the OCR candidate NGC 7193 .
GMOS/Gemini spectroscopy of 53 stars in the inner target region were obtained to derive radial velocities and atmospheric parameters .
We also employed photometric and proper motion data .
The analysis method consists of the following steps : ( i ) analysis of the statistical resemblance between the cluster and a set of field samples with respect to the sequences defined in colour-magnitude diagrams ( CMDs ) ; ( ii ) a 5-dimensional iteractive exclusion routine was employed to identify outliers from kinematical and positional data ; ( iii ) isochrone fitting to the K _ { s } \times ( J - K _ { s } ) CMD of the remaining stars and the dispersion of spectral types along empirical sequences in the ( J - H ) \times ( H - K _ { s } ) diagram was checked .
A group of stars was identified for which the mean heliocentric distance is compatible with that obtained via isochrone fitting and whose metallicities are compatible with each other .
Fifteen member stars observed spectroscopically were identified together with other 19 probable members .
Our results indicate that NGC 7193 is a genuine OCR , of an once very populous OC , for which the following parameters were derived : d = 501 \pm 46 pc , t = 2.5 \pm 1.2 Gyr , \langle [ Fe / H ] \rangle = -0.17 \pm 0.23 and E ( B - V ) = 0.05 \pm 0.05 .
Its luminosity and mass functions show depletion of low mass stars , confirming the OCR dynamically evolved state .