Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
The LAMOST-Kepler/K2 Medium-Resolution Spectroscopic Survey (LK-MRS) conducted time-domain (TD) medium-resolution spectroscopic observations of 20 LAMOST plates in the Kepler and K2 fields from 2018 to 2023, a phase designated as LK-MRS-I. A catalog of stellar parameters for a total of 36,588 stars,...
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IOP Publishing
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/adf1a9 |
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| author | Mingfeng Qin Jian-Ning Fu Weikai Zong Peter De Cat Antonio Frasca Tianqi Cang Jiangtao Wang Jianrong Shi Ali Luo Haotong Zhang Hongliang Yan J. Molenda-Żakowicz R. O. Gray Jiaxin Wang |
| author_facet | Mingfeng Qin Jian-Ning Fu Weikai Zong Peter De Cat Antonio Frasca Tianqi Cang Jiangtao Wang Jianrong Shi Ali Luo Haotong Zhang Hongliang Yan J. Molenda-Żakowicz R. O. Gray Jiaxin Wang |
| author_sort | Mingfeng Qin |
| collection | DOAJ |
| description | The LAMOST-Kepler/K2 Medium-Resolution Spectroscopic Survey (LK-MRS) conducted time-domain (TD) medium-resolution spectroscopic observations of 20 LAMOST plates in the Kepler and K2 fields from 2018 to 2023, a phase designated as LK-MRS-I. A catalog of stellar parameters for a total of 36,588 stars, derived from the spectra collected during these 5 yr, including the effective temperature, the surface gravity, the metallicity, the α -element abundance, the radial velocity (RV), and $v\sin i$ of the target stars, is released, together with the weighted averages and uncertainties. At a signal-to-noise ratio = 10, the measurement uncertainties are 120 K, 0.18 dex, 0.13 dex, 0.08 dex, 1.9 km s ^−1 , and 4.0 km s ^−1 for the above parameters, respectively. Comparisons with the parameters provided by the APOGEE and GALAH surveys validate the effective temperature and surface gravity measurements, showing minor discrepancies in metallicity and α -element abundance values. We identified some peculiar star candidates, including 764 metal-poor stars, 174 very metal-poor stars, and 30 high-velocity stars. Moreover, we found 2333 stars whose RV seems to be variable. Using Kepler/K2 or TESS photometric data, we confirmed 371 periodic variable stars among the RV variable candidates and classified their variability types. LK-MRS-I provides spectroscopic data that is useful for studies of the Kepler and K2 fields. The LK-MRS project will continue collecting TD medium-resolution spectra for target stars during the third phase of LAMOST surveys, providing data to support further scientific research. |
| format | Article |
| id | doaj-art-953a031971ba4d6d8f85ea0cd52e6c12 |
| institution | Kabale University |
| issn | 0067-0049 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Supplement Series |
| spelling | doaj-art-953a031971ba4d6d8f85ea0cd52e6c122025-08-21T06:44:01ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-0128011910.3847/1538-4365/adf1a9Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023Mingfeng Qin0https://orcid.org/0000-0002-0040-8351Jian-Ning Fu1https://orcid.org/0000-0001-8241-1740Weikai Zong2https://orcid.org/0000-0002-7660-9803Peter De Cat3https://orcid.org/0000-0001-5419-2042Antonio Frasca4https://orcid.org/0000-0002-0474-0896Tianqi Cang5https://orcid.org/0000-0003-3816-7335Jiangtao Wang6https://orcid.org/0000-0002-2316-8194Jianrong Shi7https://orcid.org/0000-0002-0349-7839Ali Luo8https://orcid.org/0000-0001-7865-2648Haotong Zhang9Hongliang Yan10https://orcid.org/0000-0002-8609-3599J. Molenda-Żakowicz11R. O. Gray12https://orcid.org/0000-0001-7588-0477Jiaxin Wang13Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; jnfu@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; jnfu@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of China; Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, Xinjiang, People’s Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; jnfu@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaRoyal Observatory of Belgium , Ringlaan 3, B-1180 Brussels, BelgiumINAF—Osservatorio Astrofisico di Catania , Via S. Sofia 78, I-95123 Catania, ItalyInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; jnfu@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of ChinaKey Lab for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of ChinaKey Lab for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of ChinaKey Lab for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of ChinaKey Lab for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of ChinaAstronomical Institute of the University of Wrocław , ul. Kopernika 11, 51-622 Wrocław, PolandDepartment of Physics and Astronomy, Appalachian State University , Boone, NC 28608, USASchool of Science, Chongqing University of Posts and Telecommunications, Chongqing 400065, People’s Republic of ChinaThe LAMOST-Kepler/K2 Medium-Resolution Spectroscopic Survey (LK-MRS) conducted time-domain (TD) medium-resolution spectroscopic observations of 20 LAMOST plates in the Kepler and K2 fields from 2018 to 2023, a phase designated as LK-MRS-I. A catalog of stellar parameters for a total of 36,588 stars, derived from the spectra collected during these 5 yr, including the effective temperature, the surface gravity, the metallicity, the α -element abundance, the radial velocity (RV), and $v\sin i$ of the target stars, is released, together with the weighted averages and uncertainties. At a signal-to-noise ratio = 10, the measurement uncertainties are 120 K, 0.18 dex, 0.13 dex, 0.08 dex, 1.9 km s ^−1 , and 4.0 km s ^−1 for the above parameters, respectively. Comparisons with the parameters provided by the APOGEE and GALAH surveys validate the effective temperature and surface gravity measurements, showing minor discrepancies in metallicity and α -element abundance values. We identified some peculiar star candidates, including 764 metal-poor stars, 174 very metal-poor stars, and 30 high-velocity stars. Moreover, we found 2333 stars whose RV seems to be variable. Using Kepler/K2 or TESS photometric data, we confirmed 371 periodic variable stars among the RV variable candidates and classified their variability types. LK-MRS-I provides spectroscopic data that is useful for studies of the Kepler and K2 fields. The LK-MRS project will continue collecting TD medium-resolution spectra for target stars during the third phase of LAMOST surveys, providing data to support further scientific research.https://doi.org/10.3847/1538-4365/adf1a9SpectroscopyCatalogsSurveysAstronomy databasesFundamental parameters of stars |
| spellingShingle | Mingfeng Qin Jian-Ning Fu Weikai Zong Peter De Cat Antonio Frasca Tianqi Cang Jiangtao Wang Jianrong Shi Ali Luo Haotong Zhang Hongliang Yan J. Molenda-Żakowicz R. O. Gray Jiaxin Wang Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023 The Astrophysical Journal Supplement Series Spectroscopy Catalogs Surveys Astronomy databases Fundamental parameters of stars |
| title | Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023 |
| title_full | Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023 |
| title_fullStr | Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023 |
| title_full_unstemmed | Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023 |
| title_short | Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023 |
| title_sort | phase ii of the lamost kepler k2 survey ii time domain of medium resolution spectroscopic observations from 2018 to 2023 |
| topic | Spectroscopy Catalogs Surveys Astronomy databases Fundamental parameters of stars |
| url | https://doi.org/10.3847/1538-4365/adf1a9 |
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