2025AJ....170..149K

A detailed analysis of the structural, astrophysical, kinematic, and dynamical properties of the open clusters Roslund 3 and Ruprecht 174 is carried out using CCD UBV photometry in conjunction with astrometric and photometric data from Gaia DR3. Membership probabilities were computed via the UPMASK algorithm applied to Gaia proper motions and trigonometric parallaxes, leading to the identification of 198 likely members for Roslund 3 and 397 for Ruprecht 174. Astrophysical parameters were derived using both the classical approach, where parameters are independently determined, and a Markov chain Monte Carlo technique, which estimates them simultaneously. The agreement between the results from both methods confirms their reliability and highlights the robustness of the classical method. The reddening values were determined as E(B - V) = 0.410 ± 0.046 mag for Roslund 3 and E(B - V) = 0.615 ± 0.042 mag for Ruprecht 174. The estimated distances are d = 1687 ± 121 pc for Roslund 3 and d = 2385 ± 163 pc for Ruprecht 174. Both clusters exhibit metallicities close to the solar value, with [Fe/H] = 0.030 ± 0.065 dex for Roslund 3 and [Fe/H] = 0.041 ± 0.064 dex for Ruprecht 174. The corresponding ages were found to be τ = 60 ± 6 and τ = 520 ± 50 Myr, respectively. The present-day mass function slopes were found to be 1.18 ± 0.13 for Roslund 3 and 1.53 ± 0.30 for Ruprecht 174, consistent with the canonical Salpeter value within uncertainties. Galactic orbital analyses indicate that both clusters are thin-disk members confined within the Solar circle. Additionally, relaxation times and spatial distributions of stars suggest that both clusters have reached dynamical relaxation and exhibit clear signs of mass segregation.