Atmospheric Parameters and Kinematic Information for the M Giant Stars from LAMOST DR9

• Published in: Research in astronomy and astrophysics Vol. 23; no. 5; pp. 55008 - 90
• Main Authors: Qiu, Dan, Tian, Hao, Li, Jing, Liu, Chao, Long, Lin, Shi, Jian-Rong, Yang, Ming, Zhang, Bo
• Format: Journal Article
• Language: English
• Published: Beijing National Astromonical Observatories, CAS and IOP Publishing 01.05.2023; IOP Publishing; Key Laboratory of Space Astronomy and Technology,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China; Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China%Key Laboratory of Space Astronomy and Technology,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China; University of Chinese Academy of Sciences,100049,China%Institute for Frontiers in Astronomy and Astrophysics,Beijing Normal University,Beijing 102206,China; Key Laboratory of Space Astronomy and Technology,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China%School of Physics and Astronomy,China West Normal University,Nanchong 637002,China%University of Chinese Academy of Sciences,100049,China
• Subjects: Apogees; Cross correlation; Galaxy: disk; Giant stars; Kinematics; Mathematical analysis; methods: data analysis; Parameters; Spectra; Stars; stars: abundances; stars: atmospheres; Uncertainty; Velocity; stars:atmospheres-Galaxy:disk; stars:abundances; methods:data analysis
• ISSN: 1674-4527; 2397-6209
• DOI: 10.1088/1674-4527/acc153

Abstract A catalog of more than 43,000 M giant stars has been selected by Li et al. from the ninth data release of LAMOST. Using the data-driven method SLAM, we obtain the stellar parameters ( T eff , log g , [M/H], [ α /M]) for all the M giant stars with uncertainties of 57 K, 0.25 dex, 0.16 dex and 0.06 dex at SNR > 100, respectively. With those stellar parameters, we constrain the absolute magnitude in the K − band, which brings distance with relative uncertainties around 25% statistically. Radial velocities are also calculated by applying cross correlation on the spectra between 8000 and 8950 Å with synthetic spectra from ATLAS9, which covers the Ca ii triplet. Comparison between our radial velocities and those from APOGEE DR17 and Gaia DR3 shows that our radial velocities have a system offset and dispersion around 1 and 4.6 km s −1 , respectively. With the distances and radial velocities combining with the astrometric data from Gaia DR3, we calculate the full 6D position and velocity information, which are able to be used for further chemo-dynamic studies on the disk and substructures in the halo, especially the Sagittarius Stream.