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Detailed analysis of the NGC 2168 cluster, leveraging Gaia DR3.

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Title: Detailed analysis of the NGC 2168 cluster, leveraging Gaia DR3.
Authors: Ahmed, Nasser M.1 (AUTHOR) nasser_ahnmed@yahoo.com, Canbay, Remziye2 (AUTHOR) rmzycnby@gmail.com, Çınar, Deniz Cennet3 (AUTHOR) denizcennetcinar@gmail.com
Source: Advances in Space Research. May2026, Vol. 77 Issue 10, p10870-10888. 19p.
Subjects: Star clusters, GAIA (Artificial satellite), Distribution of stars, Stellar evolution, Orbital mechanics, Astronomical surveys, Kinematics
Abstract: 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 ≈ 1397), with mean proper motion components of μ α cos δ = 2.278 ± 0.006 mas yr - 1 and μ δ = - 2.893 ± 0.006 mas yr - 1 , along with a mean trigonometric parallax of ϖ = 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 ] ≈ - 0.048 dex , and a probabilistic distance of 840 ± 54 pc. The radial density profile is well described by a generalized King model with β = 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. [ABSTRACT FROM AUTHOR]
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Abstract: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 ≈ 1397), with mean proper motion components of μ α cos δ = 2.278 ± 0.006 mas yr - 1 and μ δ = - 2.893 ± 0.006 mas yr - 1 , along with a mean trigonometric parallax of ϖ = 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 ] ≈ - 0.048 dex , and a probabilistic distance of 840 ± 54 pc. The radial density profile is well described by a generalized King model with β = 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. [ABSTRACT FROM AUTHOR]
ISSN:02731177
DOI:10.1016/j.asr.2026.03.061