Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
M giants, with their distinctive properties such as high luminosity, serve as excellent indicators for mapping the structure of the Milky Way. The distance to distant M giants can be determined by using the color–magnitude relation (CMR), which is derived from color–magnitude diagrams of specific sy...
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2025-01-01
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| Series: | The Astrophysical Journal Supplement Series |
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| Online Access: | https://doi.org/10.3847/1538-4365/ad9f39 |
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| author | X. Y. Tang C. J. Hao J. Li Z. Z. Yan Y. Xu J. Zhong Z. H. Lin Y. J. Li D. J. Liu L. F. Ding X. F. Long |
| author_facet | X. Y. Tang C. J. Hao J. Li Z. Z. Yan Y. Xu J. Zhong Z. H. Lin Y. J. Li D. J. Liu L. F. Ding X. F. Long |
| author_sort | X. Y. Tang |
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| description | M giants, with their distinctive properties such as high luminosity, serve as excellent indicators for mapping the structure of the Milky Way. The distance to distant M giants can be determined by using the color–magnitude relation (CMR), which is derived from color–magnitude diagrams of specific systems in previous studies. In this work, we aimed to achieve more accurate distance determination for M giants by focusing on open clusters (OCs) with a large number of member stars and thus improve the CMR. For the first time, we compiled a census of OCs harboring M giants using Gaia Data Release 3 (DR3) and Large Sky Area Multi-Object Fiber Spectroscopic Telescope Data Release 9. We identified 58 M giants associated with 43 OCs and obtained their astrometric and photometric parameters from Gaia DR3. Using the distances of these OCs, we derived the CMR for M giants as a linear correlation, expressed as ${M}_{{K}_{s}}=3.85-8.26(J-{K}_{s})$ . This linear relation proved superior to the empirical distance relation in characterizing the CMR of M giants. The photometric distances of M giants derived from the CMR are consistent with the parallax distances from Gaia and known spectroscopic distances, with median deviations of 1.5% and 2.3%, respectively. Using the distances of M giants derived from the CMR, we computed their radial velocity ( V _R ), azimuthal velocity ( V _ϕ ), and vertical velocity ( V _Z ), respectively. The distributions of these velocities revealed key features of the Galactic disk, including oscillation, north–south rotational asymmetry, and warp. These findings are consistent with previous studies and further validate the reliability of the derived CMR. |
| format | Article |
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| institution | Kabale University |
| issn | 0067-0049 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Supplement Series |
| spelling | doaj-art-767f9766f4c6463e903298b4466c702c2025-02-03T06:47:36ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-0127626310.3847/1538-4365/ad9f39Calibrating the Color–Magnitude Relation of M Giants by Using Open ClustersX. Y. Tang0C. J. Hao1J. Li2https://orcid.org/0000-0002-4953-1545Z. Z. Yan3https://orcid.org/0000-0003-3571-6060Y. Xu4https://orcid.org/0000-0001-5602-3306J. Zhong5https://orcid.org/0000-0001-5245-0335Z. H. Lin6Y. J. Li7https://orcid.org/0000-0001-7526-0120D. J. Liu8L. F. Ding9X. F. Long10School of Physics and Astronomy, China West Normal University , 1 ShiDa Road, Nanchong 637002, People’s Republic of China ; zzyan@bao.ac.cn, lijing@shao.ac.cn; Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People’s Republic of China ; xuye@pmo.ac.cnPurple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People’s Republic of China ; xuye@pmo.ac.cnSchool of Physics and Astronomy, China West Normal University , 1 ShiDa Road, Nanchong 637002, People’s Republic of China ; zzyan@bao.ac.cn, lijing@shao.ac.cnSchool of Physics and Astronomy, China West Normal University , 1 ShiDa Road, Nanchong 637002, People’s Republic of China ; zzyan@bao.ac.cn, lijing@shao.ac.cnPurple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People’s Republic of China ; xuye@pmo.ac.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaAstrophysics Division, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of ChinaPurple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People’s Republic of China ; xuye@pmo.ac.cnPurple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People’s Republic of China ; xuye@pmo.ac.cnCollege of Science, China Three Gorges University , Yichang 443002, People’s Republic of ChinaSchool of Physics and Astronomy, China West Normal University , 1 ShiDa Road, Nanchong 637002, People’s Republic of China ; zzyan@bao.ac.cn, lijing@shao.ac.cnSchool of Physics and Astronomy, China West Normal University , 1 ShiDa Road, Nanchong 637002, People’s Republic of China ; zzyan@bao.ac.cn, lijing@shao.ac.cnM giants, with their distinctive properties such as high luminosity, serve as excellent indicators for mapping the structure of the Milky Way. The distance to distant M giants can be determined by using the color–magnitude relation (CMR), which is derived from color–magnitude diagrams of specific systems in previous studies. In this work, we aimed to achieve more accurate distance determination for M giants by focusing on open clusters (OCs) with a large number of member stars and thus improve the CMR. For the first time, we compiled a census of OCs harboring M giants using Gaia Data Release 3 (DR3) and Large Sky Area Multi-Object Fiber Spectroscopic Telescope Data Release 9. We identified 58 M giants associated with 43 OCs and obtained their astrometric and photometric parameters from Gaia DR3. Using the distances of these OCs, we derived the CMR for M giants as a linear correlation, expressed as ${M}_{{K}_{s}}=3.85-8.26(J-{K}_{s})$ . This linear relation proved superior to the empirical distance relation in characterizing the CMR of M giants. The photometric distances of M giants derived from the CMR are consistent with the parallax distances from Gaia and known spectroscopic distances, with median deviations of 1.5% and 2.3%, respectively. Using the distances of M giants derived from the CMR, we computed their radial velocity ( V _R ), azimuthal velocity ( V _ϕ ), and vertical velocity ( V _Z ), respectively. The distributions of these velocities revealed key features of the Galactic disk, including oscillation, north–south rotational asymmetry, and warp. These findings are consistent with previous studies and further validate the reliability of the derived CMR.https://doi.org/10.3847/1538-4365/ad9f39Open star clustersM giant stars |
| spellingShingle | X. Y. Tang C. J. Hao J. Li Z. Z. Yan Y. Xu J. Zhong Z. H. Lin Y. J. Li D. J. Liu L. F. Ding X. F. Long Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters The Astrophysical Journal Supplement Series Open star clusters M giant stars |
| title | Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters |
| title_full | Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters |
| title_fullStr | Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters |
| title_full_unstemmed | Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters |
| title_short | Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters |
| title_sort | calibrating the color magnitude relation of m giants by using open clusters |
| topic | Open star clusters M giant stars |
| url | https://doi.org/10.3847/1538-4365/ad9f39 |
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