Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis

We conducted a photometric and kinematic analysis of the young open cluster NGC 2345 using CCD UBV data from 2-m Himalayan Chandra Telescope (HCT), Gaia Data Release 3 (DR3), 2MASS, and the APASS datasets. We found 1732 most probable cluster members with membership probability higher than 70%. The fundamental and structural parameters of the cluster are determined based on the cluster members. The mean proper motion of the cluster is estimated to be μ_αcosδ = -1.34±0.20 and μ_δ= 1.35± 0.21 mas yr^-1. Based on the radial density profile, the estimated radius is ∼ 12.8 arcmin (10.37 pc). Using color-color and color-magnitude diagrams, we estimate the reddening, age, and distance to be 0.63±0.04 mag, 63 ± 8 Myr, and 2.78 ± 0.78 kpc, respectively. The mass function slope for main-sequence stars is determined as 1.2± 0.1. The mass function slope in the core, halo, and overall region indicates a possible hint of mass segregation. The cluster's dynamical relaxation time is 177.6 Myr, meaning ongoing mass segregation, with complete equilibrium expected in 100-110 Myr. Apex coordinates are determined as -40^∘.89 ± 0.12, -44^∘.99 ± 0.15. The cluster's orbit in the Galaxy suggests early dissociation in field stars due to its close proximity to the Galactic disk.