Homogeneous Stellar Atmospheric Parameters and 22 Elemental Abundances for FGK Stars Derived from LAMOST Low-resolution Spectra with DD-PAYNE
A deep understanding of our Galaxy calls for detailed decomposition of its stellar populations via their chemical fingerprints. This requires precise stellar abundances of many elements for a large number of stars. Here, we present an updated catalog of stellar labels derived from Large Sky Area Mul...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4365/add016 |
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| author | Meng Zhang Maosheng Xiang Yuan-Sen Ting Anish Mayur Amarsi Hua-Wei Zhang Jianrong Shi Haibo Yuan Haining Li Jiahui Wang Yaqian Wu Tianmin Wu Lanya Mou Hong-Liang Yan Jifeng Liu |
| author_facet | Meng Zhang Maosheng Xiang Yuan-Sen Ting Anish Mayur Amarsi Hua-Wei Zhang Jianrong Shi Haibo Yuan Haining Li Jiahui Wang Yaqian Wu Tianmin Wu Lanya Mou Hong-Liang Yan Jifeng Liu |
| author_sort | Meng Zhang |
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| description | A deep understanding of our Galaxy calls for detailed decomposition of its stellar populations via their chemical fingerprints. This requires precise stellar abundances of many elements for a large number of stars. Here, we present an updated catalog of stellar labels derived from Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) low-resolution spectra in a physics-sensible and rigorous manner with DD-Payne , taking labels from high-resolution spectroscopy as a training set. The catalog contains atmospheric parameters for 6.4 million stars released in LAMOST DR9, and abundances for 22 elements, namely, C, N, O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Ni, Sr, Y, Zr, Ba, La, Ce, Nd, Sm, and Eu, for nearly 3.6 million stars with spectral signal-to-noise ratio (S/N) higher than 20. The [Fe/H] is valid down to ≃ −4.0, while elemental abundance ratios [X/Fe] are mostly valid for stars with [Fe/H] ≳ −2.0. Measurement errors in these labels are sensitive to and almost inversely proportional with S/N. For stars with S/N > 50, we achieved a typical error of 30 K in T _eff , 0.07 dex in $\mathrm{log}\,g$ , ∼0.05 dex in abundances for most elements with atomic number smaller than Sr, and 0.1–0.2 dex for heavier elements. Homogenization to the label estimates is carried out via dedicated internal and external calibration. In particular, the nonlocal thermal equilibrium effect is corrected for the [Fe/H] estimates, the T _eff is calibrated to the infrared flux method scale, and the $\mathrm{log}\,g$ is validated with asteroseismic measurements. The elemental abundances are internally calibrated using wide binaries, eliminating systematic trend with effective temperature. The catalog is publicly available. |
| format | Article |
| id | doaj-art-506295fa01df4faead20130c40082925 |
| institution | OA Journals |
| 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-506295fa01df4faead20130c400829252025-08-20T02:10:06ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-012791510.3847/1538-4365/add016Homogeneous Stellar Atmospheric Parameters and 22 Elemental Abundances for FGK Stars Derived from LAMOST Low-resolution Spectra with DD-PAYNEMeng Zhang0https://orcid.org/0000-0001-9293-131XMaosheng Xiang1https://orcid.org/0000-0002-5818-8769Yuan-Sen Ting2https://orcid.org/0000-0001-5082-9536Anish Mayur Amarsi3https://orcid.org/0000-0002-3181-3413Hua-Wei Zhang4https://orcid.org/0000-0002-7727-1699Jianrong Shi5Haibo Yuan6https://orcid.org/0000-0003-2471-2363Haining Li7https://orcid.org/0000-0002-0389-9264Jiahui Wang8https://orcid.org/0009-0009-3372-5271Yaqian Wu9Tianmin Wu10Lanya Mou11Hong-Liang Yan12https://orcid.org/0000-0002-8609-3599Jifeng Liu13National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cnNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cn; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of ChinaDepartment of Astronomy, The Ohio State University , Columbus, OH 45701, USA; Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University , Columbus, OH 43210, USA; Research School of Astronomy & Astrophysics, Australian National University , Cotter Road, Weston, ACT 2611, Australia; School of Computing, Australian National University , Acton, ACT 2601, AustraliaTheoretical Astrophysics, Department of Physics and Astronomy, Uppsala University , Box 516, SE-751 20, Uppsala, SwedenDepartment of Astronomy, School of Physics, Peking University , Beijing 100871, People’s Republic of China; Kavli institute of Astronomy and Astrophysics, Peking University , Beijing 100871, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China; Department of Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cnNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cnNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cn; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; zhangm@nao.cas.cn, msxiang@nao.cas.cn; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China; WHU-NAOC Joint Center for Astronomy, Wuhan University , Wuhan, Hubei 430072, People’s Republic of ChinaA deep understanding of our Galaxy calls for detailed decomposition of its stellar populations via their chemical fingerprints. This requires precise stellar abundances of many elements for a large number of stars. Here, we present an updated catalog of stellar labels derived from Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) low-resolution spectra in a physics-sensible and rigorous manner with DD-Payne , taking labels from high-resolution spectroscopy as a training set. The catalog contains atmospheric parameters for 6.4 million stars released in LAMOST DR9, and abundances for 22 elements, namely, C, N, O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Ni, Sr, Y, Zr, Ba, La, Ce, Nd, Sm, and Eu, for nearly 3.6 million stars with spectral signal-to-noise ratio (S/N) higher than 20. The [Fe/H] is valid down to ≃ −4.0, while elemental abundance ratios [X/Fe] are mostly valid for stars with [Fe/H] ≳ −2.0. Measurement errors in these labels are sensitive to and almost inversely proportional with S/N. For stars with S/N > 50, we achieved a typical error of 30 K in T _eff , 0.07 dex in $\mathrm{log}\,g$ , ∼0.05 dex in abundances for most elements with atomic number smaller than Sr, and 0.1–0.2 dex for heavier elements. Homogenization to the label estimates is carried out via dedicated internal and external calibration. In particular, the nonlocal thermal equilibrium effect is corrected for the [Fe/H] estimates, the T _eff is calibrated to the infrared flux method scale, and the $\mathrm{log}\,g$ is validated with asteroseismic measurements. The elemental abundances are internally calibrated using wide binaries, eliminating systematic trend with effective temperature. The catalog is publicly available.https://doi.org/10.3847/1538-4365/add016SurveysStellar abundancesGalaxy chemical evolutionSpectroscopyStellar physicsMilky Way evolution |
| spellingShingle | Meng Zhang Maosheng Xiang Yuan-Sen Ting Anish Mayur Amarsi Hua-Wei Zhang Jianrong Shi Haibo Yuan Haining Li Jiahui Wang Yaqian Wu Tianmin Wu Lanya Mou Hong-Liang Yan Jifeng Liu Homogeneous Stellar Atmospheric Parameters and 22 Elemental Abundances for FGK Stars Derived from LAMOST Low-resolution Spectra with DD-PAYNE The Astrophysical Journal Supplement Series Surveys Stellar abundances Galaxy chemical evolution Spectroscopy Stellar physics Milky Way evolution |
| title | Homogeneous Stellar Atmospheric Parameters and 22 Elemental Abundances for FGK Stars Derived from LAMOST Low-resolution Spectra with DD-PAYNE |
| title_full | Homogeneous Stellar Atmospheric Parameters and 22 Elemental Abundances for FGK Stars Derived from LAMOST Low-resolution Spectra with DD-PAYNE |
| title_fullStr | Homogeneous Stellar Atmospheric Parameters and 22 Elemental Abundances for FGK Stars Derived from LAMOST Low-resolution Spectra with DD-PAYNE |
| title_full_unstemmed | Homogeneous Stellar Atmospheric Parameters and 22 Elemental Abundances for FGK Stars Derived from LAMOST Low-resolution Spectra with DD-PAYNE |
| title_short | Homogeneous Stellar Atmospheric Parameters and 22 Elemental Abundances for FGK Stars Derived from LAMOST Low-resolution Spectra with DD-PAYNE |
| title_sort | homogeneous stellar atmospheric parameters and 22 elemental abundances for fgk stars derived from lamost low resolution spectra with dd payne |
| topic | Surveys Stellar abundances Galaxy chemical evolution Spectroscopy Stellar physics Milky Way evolution |
| url | https://doi.org/10.3847/1538-4365/add016 |
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