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In-depth analysis of photometric and kinematic characteristics of SAI 16, SAI 81 and SAI 86 open clusters utilizing Gaia DR3.

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Title: In-depth analysis of photometric and kinematic characteristics of SAI 16, SAI 81 and SAI 86 open clusters utilizing Gaia DR3.
Authors: Alzhrani, A. Y.1 (AUTHOR), Haroon, A. A.1 (AUTHOR), Elsanhoury, W. H.2 (AUTHOR) elsanhoury@nbu.edu.sa, Çinar, D. C.3 (AUTHOR)
Source: Journal of Astrophysics & Astronomy. 8/21/2025, Vol. 46 Issue 2, p1-18. 18p.
Subjects: Open clusters of stars, Star clusters, GAIA (Artificial satellite), Stellar dynamics, Astronomical observations, Photometry
Abstract: This study comprehensively analyses three open star clusters: SAI 16, SAI 81 and SAI 86 using Gaia DR3 data. Based on the ASteCA code, we determined the most probable star candidates ( P ≥ 50 %) and estimated the number of star members of each cluster as 125, 158 and 138, respectively. We estimated the internal structural parameters by fitting the King model to the observed radial density profiles, including the core, limited and tidal radii. Isochrone fitting to the colour–magnitude diagram provided log age of 9.13 ± 0.04 , 8.10 ± 0.04 and 8.65 ± 0.04 and distances (d) of 3790 ± 94 , 3900 ± 200 and 3120 ± 30 pc for SAI 16, SAI 81 and SAI 86, respectively. Moreover, we have calculated their projected distances from the galactic plane ( X ⊙ , Y ⊙) as well as their projected distance from the galactic plane (Z ⊙) , distance from the galactic centre ( R gc ) and total mass ( M C ) in solar units are about 142 ± 12 , 302 ± 17 and 192 ± 14 for SAI 16, SAI 81 and SAI 86, respectively. Examining the dynamical relaxation state indicates that all three clusters are dynamically relaxed. By undertaking a kinematic analysis of the cluster data, space velocity was determined. We calculated the coordinates of the apex point ( A o , D o ) using the AD diagram method along with the derivation of solar elements ( S ⊙ , l A , b A ). Through our detailed dynamic orbit analysis, we determined that the three SAI clusters belong to the young stellar disc, confirming their membership within this component of the galactic structure. [ABSTRACT FROM AUTHOR]
Copyright of Journal of Astrophysics & Astronomy is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: In-depth analysis of photometric and kinematic characteristics of SAI 16, SAI 81 and SAI 86 open clusters utilizing Gaia DR3.
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Astrophysics+%26+Astronomy%22">Journal of Astrophysics & Astronomy</searchLink>. 8/21/2025, Vol. 46 Issue 2, p1-18. 18p.
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  Data: <searchLink fieldCode="DE" term="%22Open+clusters+of+stars%22">Open clusters of stars</searchLink><br /><searchLink fieldCode="DE" term="%22Star+clusters%22">Star clusters</searchLink><br /><searchLink fieldCode="DE" term="%22GAIA+%28Artificial+satellite%29%22">GAIA (Artificial satellite)</searchLink><br /><searchLink fieldCode="DE" term="%22Stellar+dynamics%22">Stellar dynamics</searchLink><br /><searchLink fieldCode="DE" term="%22Astronomical+observations%22">Astronomical observations</searchLink><br /><searchLink fieldCode="DE" term="%22Photometry%22">Photometry</searchLink>
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  Label: Abstract
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  Data: This study comprehensively analyses three open star clusters: SAI 16, SAI 81 and SAI 86 using Gaia DR3 data. Based on the ASteCA code, we determined the most probable star candidates ( P ≥ 50 %) and estimated the number of star members of each cluster as 125, 158 and 138, respectively. We estimated the internal structural parameters by fitting the King model to the observed radial density profiles, including the core, limited and tidal radii. Isochrone fitting to the colour–magnitude diagram provided log age of 9.13 ± 0.04 , 8.10 ± 0.04 and 8.65 ± 0.04 and distances (d) of 3790 ± 94 , 3900 ± 200 and 3120 ± 30 pc for SAI 16, SAI 81 and SAI 86, respectively. Moreover, we have calculated their projected distances from the galactic plane ( X ⊙ , Y ⊙) as well as their projected distance from the galactic plane (Z ⊙) , distance from the galactic centre ( R gc ) and total mass ( M C ) in solar units are about 142 ± 12 , 302 ± 17 and 192 ± 14 for SAI 16, SAI 81 and SAI 86, respectively. Examining the dynamical relaxation state indicates that all three clusters are dynamically relaxed. By undertaking a kinematic analysis of the cluster data, space velocity was determined. We calculated the coordinates of the apex point ( A o , D o ) using the AD diagram method along with the derivation of solar elements ( S ⊙ , l A , b A ). Through our detailed dynamic orbit analysis, we determined that the three SAI clusters belong to the young stellar disc, confirming their membership within this component of the galactic structure. [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
  Label:
  Group: Ab
  Data: <i>Copyright of Journal of Astrophysics & Astronomy is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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              Text: 8/21/2025
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