APPLICATION OF THE SEGUE STELLAR PARAMETER PIPELINE TO LAMOST STELLAR SPECTRA

ABSTRACT We describe an application of the SEGUE Stellar Parameter Pipeline (SSPP) to medium-resolution stellar spectra obtained by the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST), in order to determine estimates of the stellar atmospheric parameters (Teff, , and [Fe/H]) and t...

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Bibliographic Details
Published in:The Astronomical journal 2015-12, Vol.150 (6), p.1-18
Main Authors: Lee, Young Sun, Beers, Timothy C., Carlin, Jeffrey L., Newberg, Heidi J., Hou, Yonghui, Li, Guangwei, Luo, A.-Li, Wu, Yue, Yang, Ming, Zhang, Haotong, Zhang, Wei, Zhang, Yong
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Atmospherics
COMPARATIVE EVALUATIONS
COMPUTERIZED SIMULATION
DATA ANALYSIS
GALACTIC EVOLUTION
Galactic halos
methods: data analysis
Offsets
Pipelines
RADIAL VELOCITY
RESOLUTION
SIGNAL-TO-NOISE RATIO
SPECTRA
SPECTROSCOPY
STARS
stars: abundances
Stellar spectra
techniques: imaging spectroscopy
TELESCOPES
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Summary:ABSTRACT We describe an application of the SEGUE Stellar Parameter Pipeline (SSPP) to medium-resolution stellar spectra obtained by the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST), in order to determine estimates of the stellar atmospheric parameters (Teff, , and [Fe/H]) and the abundance ratios ([ /Fe] and [C/Fe]). By performing a coordinate match with the LAMOST stellar database, we selected stars with LAMOST spectra in common with stars having available spectroscopy from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), the RAdial Velocity Experiment (RAVE), and the Sloan Extension for Galactic Understanding and Exploration (SEGUE). We ran the selected LAMOST stellar spectra from each survey through SSPP, and compared the stellar parameters down to signal-to-noise ratio (S/N) of 10 and chemical abundances down to S/N = 20 derived by SSPP with those determined by the APOGEE, RAVE, and SEGUE software pipelines. Our results show that the derived stellar parameters generally agree quite well, even though there exist some small systematic offsets with small scatter in Teff, , and [Fe/H], due to the use of different temperature scales, abundance scales, and calibrations adopted by each survey. Comparison of the [ /Fe] determinations for LAMOST spectra suggests no sign of significant systematic offsets (
ISSN:0004-6256
1538-3881
1538-3881
DOI:10.1088/0004-6256/150/6/187