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Deeply comprehensive astrometric, photometric, and kinematic studies of the three OCSN open clusters with Gaia DR3.

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Title: Deeply comprehensive astrometric, photometric, and kinematic studies of the three OCSN open clusters with Gaia DR3.
Authors: Elsanhoury, W. H.1 (AUTHOR) elsanhoury@nbu.edu.sa, Haroon, A. A.2 (AUTHOR), Elkholy, E. A.1,3 (AUTHOR), Çinar, D. C.4 (AUTHOR)
Source: Journal of Astrophysics & Astronomy. 3/19/2025, Vol. 46 Issue 1, p1-17. 17p.
Subjects: Star clusters, Data release, Orbits (Astronomy), Cluster analysis (Statistics), Kinematics
Abstract: In this study, we considered the optical wavelength of Gaia Data Release 3 (DR3) to analyze poorly studied three newly open star clusters, namely OCSN 203, OCSN 213, and OCSN 244 clusters with ASteCA code. Here, we identified 227, 200, and 551 candidates with highly probable ( P ≥ 50 %) members. Fitting King's profile within radial density profiles allows us to estimate inner stellar structures like core ( 0.190 ≤ r c (pc) ≤ 1.284 ) and the limiting ( 0.327 ≤ r cl (pc) ≤ 1.302 ) radii. Constructing color-magnitude diagrams (CMDs) fitted with suitable log age (yr) between ( log t ; 6.52–7.05) and metallicities (Z; 0.01308–0.01413) isochrones. Therefore, the estimated photometric parameters with CMDs reflect the heliocentric distances are 332 ± 18 , 529 ± 23 , and 506 ± 23 (pc) for OCSN 203, OCSN 213, and OCSN 244, respectively. Furthermore, the collective mass ( M C ) in solar mass units is calculated with MLR as 67 ± 8.19 , 91 ± 9.54 , and 353 ± 18.79 . Additionally, LF determined that the mean absolute magnitudes are 9.54 ± 3.09 , 8.52 ± 2.92 , and 7.60 ± 2.76 for these clusters, respectively. The overall mass function reflects the slopes (α ) for Salpeter within the uncertainty are ( α OCSN 203 = 2.41 ± 0.06 ), ( α OCSN 213 = 2.13 ± 0.07 ), and ( α OCSN 244 = 2.28 ± 0.07 ). The results of this study, which employed a dynamical analysis over varying timescales, indicate that OCSN 203 and OCSN 244 are clusters that have undergone significant relaxation, with a dynamical evolution parameter (τ ) that is much greater than one. In contrast, OCSN 213 exhibits characteristics of a non-relaxed cluster. A kinematic analysis of these open clusters was carried out, encompassing aspects of their apex position ( A o , D o ) using the AD diagrams. Therefore, the numerical convergent point coordinates are 76 ∘. 77 ± 0 ∘. 01 , - 0 ∘. 23 ± 0 ∘. 00 (OCSN 203), 85 ∘. 71 ± 0 ∘. 11 , - 9 ∘. 63 ± 0 ∘. 03 (OCSN 213), and 88 ∘. 19 ± 0 ∘. 11 , - 4 ∘. 04 ± 0 ∘. 01 (OCSN 244). We found that the three OCSN clusters are young stellar disc members using dynamic orbit parameters. [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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  Label: Title
  Group: Ti
  Data: Deeply comprehensive astrometric, photometric, and kinematic studies of the three OCSN open clusters with Gaia DR3.
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Astrophysics+%26+Astronomy%22">Journal of Astrophysics & Astronomy</searchLink>. 3/19/2025, Vol. 46 Issue 1, p1-17. 17p.
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  Data: <searchLink fieldCode="DE" term="%22Star+clusters%22">Star clusters</searchLink><br /><searchLink fieldCode="DE" term="%22Data+release%22">Data release</searchLink><br /><searchLink fieldCode="DE" term="%22Orbits+%28Astronomy%29%22">Orbits (Astronomy)</searchLink><br /><searchLink fieldCode="DE" term="%22Cluster+analysis+%28Statistics%29%22">Cluster analysis (Statistics)</searchLink><br /><searchLink fieldCode="DE" term="%22Kinematics%22">Kinematics</searchLink>
– Name: Abstract
  Label: Abstract
  Group: Ab
  Data: In this study, we considered the optical wavelength of Gaia Data Release 3 (DR3) to analyze poorly studied three newly open star clusters, namely OCSN 203, OCSN 213, and OCSN 244 clusters with ASteCA code. Here, we identified 227, 200, and 551 candidates with highly probable ( P ≥ 50 %) members. Fitting King's profile within radial density profiles allows us to estimate inner stellar structures like core ( 0.190 ≤ r c (pc) ≤ 1.284 ) and the limiting ( 0.327 ≤ r cl (pc) ≤ 1.302 ) radii. Constructing color-magnitude diagrams (CMDs) fitted with suitable log age (yr) between ( log t ; 6.52–7.05) and metallicities (Z; 0.01308–0.01413) isochrones. Therefore, the estimated photometric parameters with CMDs reflect the heliocentric distances are 332 ± 18 , 529 ± 23 , and 506 ± 23 (pc) for OCSN 203, OCSN 213, and OCSN 244, respectively. Furthermore, the collective mass ( M C ) in solar mass units is calculated with MLR as 67 ± 8.19 , 91 ± 9.54 , and 353 ± 18.79 . Additionally, LF determined that the mean absolute magnitudes are 9.54 ± 3.09 , 8.52 ± 2.92 , and 7.60 ± 2.76 for these clusters, respectively. The overall mass function reflects the slopes (α ) for Salpeter within the uncertainty are ( α OCSN 203 = 2.41 ± 0.06 ), ( α OCSN 213 = 2.13 ± 0.07 ), and ( α OCSN 244 = 2.28 ± 0.07 ). The results of this study, which employed a dynamical analysis over varying timescales, indicate that OCSN 203 and OCSN 244 are clusters that have undergone significant relaxation, with a dynamical evolution parameter (τ ) that is much greater than one. In contrast, OCSN 213 exhibits characteristics of a non-relaxed cluster. A kinematic analysis of these open clusters was carried out, encompassing aspects of their apex position ( A o , D o ) using the AD diagrams. Therefore, the numerical convergent point coordinates are 76 ∘. 77 ± 0 ∘. 01 , - 0 ∘. 23 ± 0 ∘. 00 (OCSN 203), 85 ∘. 71 ± 0 ∘. 11 , - 9 ∘. 63 ± 0 ∘. 03 (OCSN 213), and 88 ∘. 19 ± 0 ∘. 11 , - 4 ∘. 04 ± 0 ∘. 01 (OCSN 244). We found that the three OCSN clusters are young stellar disc members using dynamic orbit parameters. [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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        Value: 10.1007/s12036-025-10044-0
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      – Code: eng
        Text: English
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        PageCount: 17
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      – SubjectFull: Star clusters
        Type: general
      – SubjectFull: Data release
        Type: general
      – SubjectFull: Orbits (Astronomy)
        Type: general
      – SubjectFull: Cluster analysis (Statistics)
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      – SubjectFull: Kinematics
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      – TitleFull: Deeply comprehensive astrometric, photometric, and kinematic studies of the three OCSN open clusters with Gaia DR3.
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              Text: 3/19/2025
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