Deeply comprehensive astrometric, photometric, and kinematic studies of the three OCSN open clusters with Gaia DR3

Abstract

In this study, we considered the optical wavelength of Gaia Data Release 3 (DR3) to analyze poorly studied three newly open star clusters, namely OCSN 203, OCSN 213, and OCSN 244 clusters with ASteCA code. Here, we identified 227, 200, and 551 candidates with highly probable (\(P \ge 50\)%) members. Fitting King’s profile within radial density profiles allows us to estimate inner stellar structures like core (\(0.190 \le r_{\textrm{c}} \ \mathrm{(pc)} \le 1.284\)) and the limiting (\(0.327 \le r_{\textrm{cl}} \ \mathrm{(pc)} \le 1.302\)) radii. Constructing color-magnitude diagrams (CMDs) fitted with suitable \(\log \textrm{age}\) (yr) between (\(\log t\); 6.52–7.05) and metallicities (Z; 0.01308–0.01413) isochrones. Therefore, the estimated photometric parameters with CMDs reflect the heliocentric distances are \(332 \pm 18\), \(529 \pm 23\), and \(506 \pm 23\) (pc) for OCSN 203, OCSN 213, and OCSN 244, respectively. Furthermore, the collective mass (\(M_{C}\)) in solar mass units is calculated with MLR as \(67 \pm 8.19\), \(91 \pm 9.54\), and \(353 \pm 18.79\). Additionally, LF determined that the mean absolute magnitudes are \(9.54 \pm 3.09\), \(8.52 \pm 2.92\), and \(7.60 \pm 2.76\) for these clusters, respectively. The overall mass function reflects the slopes (\(\alpha \)) for Salpeter within the uncertainty are (\(\alpha _{\mathrm{OCSN \ 203}} = 2.41 \pm 0.06\)), (\(\alpha _{\mathrm{OCSN \ 213}} = 2.13 \pm 0.07\)), and (\(\alpha _{\mathrm{OCSN \ 244}} = 2.28 \pm 0.07\)). The results of this study, which employed a dynamical analysis over varying timescales, indicate that OCSN 203 and OCSN 244 are clusters that have undergone significant relaxation, with a dynamical evolution parameter (\(\tau \)) that is much greater than one. In contrast, OCSN 213 exhibits characteristics of a non-relaxed cluster. A kinematic analysis of these open clusters was carried out, encompassing aspects of their apex position (\(A_{\textrm{o}}, D_{\textrm{o}}\)) using the AD diagrams. Therefore, the numerical convergent point coordinates are \(76^{\circ }.77 \pm 0^{\circ }.01\), \(-0^{\circ }.23 \pm 0^{\circ }.00\) (OCSN 203), \(85^{\circ }.71 \pm 0^{\circ }.11\), \(-9^{\circ }.63 \pm 0^{\circ }.03\) (OCSN 213), and \(88^{\circ }.19 \pm 0^{\circ }.11\), \(-4^{\circ }.04 \pm 0^{\circ }.01\) (OCSN 244). We found that the three OCSN clusters are young stellar disc members using dynamic orbit parameters.