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Detailed analysis of the NGC 2168 cluster, leveraging Gaia DR3
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DOI：10.1016/j.asr.2026.03.061.png)
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Abstract
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NGC 2168 (M35) serves as a fundamental benchmark for studying stellar evolution and dynamical environments at the transition between young and intermediate-age populations. We present a comprehensive analysis of the cluster's kinematic, structural, and astrophysical properties utilizing high-precision astrometry and photometry data from Gaia Data Release 3 (DR3), complemented by 2MASS data. A statistical membership assessment yields a clean sample of probable members (N approximate to 1397), with mean proper motion components of & micro;(alpha) cos delta = 2 278 0 006 mas yr (-1 )and & micro;(delta) =2 893 +/- 0.006 mas yr (-1), along with a mean trigonometric parallax of Pi= 1 154 +/- 0. 052 mas. We derived the cluster's fundamental parameters via isochrone fitting, determining an age of 190 +/- 12 Myr, a metallicity of [M/ H ]approximate to -0 048 dex, and a probabilistic distance of 840 +/- 54 pc. The radial density profile is well described by a generalized King model with beta =1 (r(c) =7 97', r(cl )=36 .69'), revealing the presence of a loosely bound, extended stellar halo. Furthermore, we detect a spatial elongation oriented perpendicular to the Galactic plane, likely a signature of vertical tidal heating or disk shocking. The mass function analysis exhibits a multimodal Gaussian structure, suggesting a complex dynamical formation history beyond a simple power-law distribution. Finally, orbital integration confirms NGC 2168 as a thin disk object with a maximum vertical excursion of 171 pc, consistent with the observed vertical morphological deformation. (c) 2026 COSPAR. Published by Elsevier B.V. All rights are reserved, including those for text and data mining, AI training, and similar technologies.
Keywords:
Open clusters and associations: individual: NGC 2168
Galaxy: kinematics and dynamics
Astrometry
Stars: Hertzsprung-Russell and C-M diagrams
Methods: statistical
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