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Galactic open clusters (OCs) that survive the early gas-expulsion phase aregradually destroyed over time by the action of disruptive dynamical processes.Their final evolutionary stages are characterized by a poorly populatedconcentration of stars called open cluster remnant (OCR). This study is devotedto assess the real physical nature of the OCR candidate NGC 7193. GMOS/Geminispectroscopy of 53 stars in the inner target region were obtained to deriveradial velocities and atmospheric parameters. We also employed photometric andproper motion data. The analysis method consists of the following steps: (i)analysis of the statistical resemblance between the cluster and a set of fieldsamples with respect to the sequences defined in colour-magnitude diagrams(CMDs); (ii) a 5-dimensional iteractive exclusion routine was employed toidentify outliers from kinematical and positional data; (iii) isochrone fittingto the $K_{s}\times(J-K_{s})$ CMD of the remaining stars and the dispersion ofspectral types along empirical sequences in the $(J-H)\times(H-K_{s})$ diagramwas checked. A group of stars was identified for which the mean heliocentricdistance is compatible with that obtained via isochrone fitting and whosemetallicities are compatible with each other. Fifteen member stars observedspectroscopically were identified together with other 19 probable members. Ourresults 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 oflow mass stars, confirming the OCR dynamically evolved state.

Investigation of Galactic open cluster remnants: the case of NGC 7193