dc.contributor.author |
Belwal, Kuldeep |
|
dc.contributor.author |
Bisht, D |
|
dc.contributor.author |
Bisht, Mohit Singh |
|
dc.contributor.author |
Rangwal, Geeta |
|
dc.contributor.author |
Raj, Ashish |
|
dc.contributor.author |
Dattatrey, Arvind K |
|
dc.contributor.author |
Yadav, R. K. S |
|
dc.contributor.author |
Bhatt, B. C |
|
dc.date.accessioned |
2024-06-21T03:55:07Z |
|
dc.date.available |
2024-06-21T03:55:07Z |
|
dc.date.issued |
2024-05-01 |
|
dc.identifier.citation |
The Astronomical Journal, Vol. 167, No. 5, 188 |
en_US |
dc.identifier.issn |
1538-3881 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/8478 |
|
dc.description |
Open Access. |
en_US |
dc.description |
Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. |
|
dc.description.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. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
American Astronomical Society |
en_US |
dc.relation.uri |
https://doi.org/10.3847/1538-3881/ad2fcc |
|
dc.rights |
© 2024. The Author(s) |
|
dc.subject |
Open star clusters |
en_US |
dc.subject |
Orbits |
en_US |
dc.subject |
Initial mass function |
en_US |
dc.subject |
Interstellar extinction |
en_US |
dc.title |
Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis |
en_US |
dc.type |
Article |
en_US |