2025MNRAS.536..174S

We present a statistical and multiwavelength photometric study of the young open cluster NGC 6193. To determine cluster membership, we used an unsupervised ensemble-based machine-learning approach and identified 246 cluster members with a search radius of 30 arcmin using $Gaia$ DR3 astrometry data. From isochrone fitting using ASTECA, we found that NGC 6193 is a very young open cluster with an age of 4.22 Myr at a distance of 1.295 Kpc having metallicity, z$\sim$ 0.023 and an extinction of $A_v$$\sim$ 1.452. We analysed the mass function (MF) for NGC 6193 using the Monte Carlo method. The MF is found to be segmented at mass $\sim$0.69 M$_{\odot }$ and MF slope for the low-mass end, $\Gamma _\mathit{ B}$ = 2.09, and for the high-mass end $\Gamma _\mathit{ A}$ = -1.09. The young stellar objects (YSOs) have been identified using the $(J-H)\ \mathrm{ versus}\ (H-K)$ colour-colour diagram and the identified YSOs have masses 0.15 to 6.0 M$_{\odot }$ and ages $\le$3 Myr. We determined the extinction using the PNICER technique, which is found to be consistent with the dust structure obtained from the 22 $\mu \mathrm{m}$ dust continuum emissions map of WISE for the cluster region. We found that NGC 6193 is a dynamically young cluster with mass segregation, which may have resulted from either primordial star formation processes or early dynamical evolution. We also performed orbit analysis using GALPY and the cluster is found to be within the solar circle. Finally, at the end, we discussed the star formation scenario in the cluster region.