Abstract:
We conducted a photometric and kinematic analysis of the young open cluster NGC 2345 using CCD UBV data
from 2 m Himalayan Chandra Telescope, Gaia Data Release 3, Two Micron All-Sky Survey, and the Photometric
All-Sky Survey data sets. 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 m d a cos = −1.34 ± 0.20 and μδ = 1.35 ± 0.21 mas yr−1
.
Based on the radial density profile, the estimated radius is ∼12 8 (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 into field stars due to its close proximity to the Galactic disk.
