Structure and evolution of multi-cluster within Galactic disc: Gaia DR3 insights into eight open clusters
Journal of Astrophysics and Astronomy, cilt.47, sa.1, 2026 (SCI-Expanded, Scopus)
- Yayın Türü: Makale / Tam Makale
- Cilt numarası: 47 Sayı: 1
- Basım Tarihi: 2026
- Doi Numarası: 10.1007/s12036-026-10143-6
- Dergi Adı: Journal of Astrophysics and Astronomy
- Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Aerospace Database, INSPEC, Academic Search Ultimate (EBSCO), Natural Science Collection (ProQuest), Earth, Atmospheric, & Aquatic Science Collection (ProQuest), Engineering Source (EBSCO), Technology Collection (ProQuest)
- Anahtar Kelimeler: astrometric, colour magnitude diagrams, galactic orbit parameters, kinematics, Open clusters
- İstanbul Üniversitesi Adresli: Evet
Özet
In this study, we present a comprehensive analysis of the structural, astrophysical, and dynamical properties of eight open clusters: NGC 559, NGC 1817, NGC 2141, NGC 7245, Ruprecht 15, Ruprecht 137, Ruprecht 142, and Ruprecht 169, utilizing the precise astrometric and photometric data from Gaia Data Release 3. By fitting King’s model to the radial density profiles, we determined their structural parameters, including core and cluster limiting radii, which were found to be in the ranges of 3.07 – 16.21 arcmin and 9.97 – 25.97 arcmin, respectively. The fundamental astrophysical parameters were derived by fitting PARSEC isochrones to the colour-magnitude diagrams. Our analysis indicates that the clusters’ logarithmic ages span from 7.95 to 9.34 years, with metallicities ranging between 0.007 – 0.015 and heliocentric distances from 1640 to 5203 pc. The total stellar masses for the clusters were calculated to be within the range of 257 – 1916 M⊙. The slopes of the mass function for most clusters were found to be consistent with the Salpeter initial mass function. Furthermore, our dynamical analysis suggests that all investigated clusters except Ruprecht 15 show signs of being dynamically relaxed. Notably, the spatial distribution and bimodal structure observed in the radial density profile of NGC 7245 provide strong evidence that it is a binary cluster candidate. Finally, our kinematic analysis and orbit integration show that the clusters possess dynamical properties that are fully consistent with their membership in the Galactic thin disc.