Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
We present a multimethod investigation of four metal-poor G-type main-sequence stars to resolve their Galactic origins. By combining high-resolution spectroscopy from PolarBase, photometric/astrometric data from Gaia DR3, and spectral energy distribution modeling, we derive precise stellar parameter...
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IOP Publishing
2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-3881/add343 |
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| author | Deniz Cennet Çınar Selçuk Bilir Timur Şahin Olcay Plevne |
| author_facet | Deniz Cennet Çınar Selçuk Bilir Timur Şahin Olcay Plevne |
| author_sort | Deniz Cennet Çınar |
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| description | We present a multimethod investigation of four metal-poor G-type main-sequence stars to resolve their Galactic origins. By combining high-resolution spectroscopy from PolarBase, photometric/astrometric data from Gaia DR3, and spectral energy distribution modeling, we derive precise stellar parameters, chemical abundances, kinematics, and Galactic orbital parameters. The stars HD 22879, HD 144579, HD 188510, and HD 201891 show effective temperatures of 5855 ± 110, 5300 ± 160, 5370 ± 60, and 5880 ± 90 K; surface gravities of 4.40 ± 0.18, 4.52 ± 0.37, 4.57 ± 0.13, and 4.48 ± 0.18 cgs; and metallicities of −0.86 ± 0.08, −0.55 ± 0.12, −1.60 ± 0.07, and −1.15 ± 0.07 dex, respectively. Kinematic analysis suggests that HD 22879, HD 144579, and HD 201891 are potential bulge-origin escapees, possibly ejected by the Galactic bar or spiral arm perturbations. HD 188510, however, shows halo-like dynamics, including a retrograde orbit. Chemical abundance trends ([ α /Fe] versus [Fe/H]) reveal mixed origins, challenging kinematic classifications. This discrepancy highlights the importance of integrative methodologies in Galactic archaeology. We associate HD 22879, HD 144579, and HD 201891 with the bulge globular cluster NGC 6441, NGC 5927, and NGC 6544, respectively. HD 188510’s retrograde motion and low metallicity align with ejection from the halo globular cluster NGC 5139 ( ω Cen). These results illustrate the complex interplay of dynamical processes—including bar resonances, spiral arm perturbations, and tidal stripping—in depositing metal-poor stars into the solar neighborhood. |
| format | Article |
| id | doaj-art-9752d4642975438aac824d47e690d44e |
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| issn | 1538-3881 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj-art-9752d4642975438aac824d47e690d44e2025-08-20T02:32:08ZengIOP PublishingThe Astronomical Journal1538-38812025-01-0117011310.3847/1538-3881/add343Tracing the Galactic Origins of Selected Four G-type Stars in the Solar NeighborhoodDeniz Cennet Çınar0https://orcid.org/0000-0001-7940-3731Selçuk Bilir1https://orcid.org/0000-0003-3510-1509Timur Şahin2https://orcid.org/0000-0002-0296-233XOlcay Plevne3https://orcid.org/0000-0002-0435-4493Programme of Astronomy and Space Sciences , Institute of Graduate Studies in Science, Istanbul University, 34116, Istanbul, Türkiye ; denizcdursun@gmail.comDepartment of Astronomy and Space Sciences , Faculty of Science, Istanbul University, 34119, Istanbul, TürkiyeDepartment of Space Sciences and Technologies , Faculty of Science, Akdeniz University, 07058, Antalya, TürkiyeDepartment of Astronomy and Space Sciences , Faculty of Science, Istanbul University, 34119, Istanbul, TürkiyeWe present a multimethod investigation of four metal-poor G-type main-sequence stars to resolve their Galactic origins. By combining high-resolution spectroscopy from PolarBase, photometric/astrometric data from Gaia DR3, and spectral energy distribution modeling, we derive precise stellar parameters, chemical abundances, kinematics, and Galactic orbital parameters. The stars HD 22879, HD 144579, HD 188510, and HD 201891 show effective temperatures of 5855 ± 110, 5300 ± 160, 5370 ± 60, and 5880 ± 90 K; surface gravities of 4.40 ± 0.18, 4.52 ± 0.37, 4.57 ± 0.13, and 4.48 ± 0.18 cgs; and metallicities of −0.86 ± 0.08, −0.55 ± 0.12, −1.60 ± 0.07, and −1.15 ± 0.07 dex, respectively. Kinematic analysis suggests that HD 22879, HD 144579, and HD 201891 are potential bulge-origin escapees, possibly ejected by the Galactic bar or spiral arm perturbations. HD 188510, however, shows halo-like dynamics, including a retrograde orbit. Chemical abundance trends ([ α /Fe] versus [Fe/H]) reveal mixed origins, challenging kinematic classifications. This discrepancy highlights the importance of integrative methodologies in Galactic archaeology. We associate HD 22879, HD 144579, and HD 201891 with the bulge globular cluster NGC 6441, NGC 5927, and NGC 6544, respectively. HD 188510’s retrograde motion and low metallicity align with ejection from the halo globular cluster NGC 5139 ( ω Cen). These results illustrate the complex interplay of dynamical processes—including bar resonances, spiral arm perturbations, and tidal stripping—in depositing metal-poor stars into the solar neighborhood.https://doi.org/10.3847/1538-3881/add343Solar neighborhoodChemical abundancesStellar kinematicsStellar dynamics |
| spellingShingle | Deniz Cennet Çınar Selçuk Bilir Timur Şahin Olcay Plevne Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood The Astronomical Journal Solar neighborhood Chemical abundances Stellar kinematics Stellar dynamics |
| title | Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood |
| title_full | Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood |
| title_fullStr | Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood |
| title_full_unstemmed | Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood |
| title_short | Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood |
| title_sort | tracing the galactic origins of selected four g type stars in the solar neighborhood |
| topic | Solar neighborhood Chemical abundances Stellar kinematics Stellar dynamics |
| url | https://doi.org/10.3847/1538-3881/add343 |
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