LAMOST Observations in 15 K2 Campaigns. I. Low-resolution Spectra from LAMOST DR6
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Author
Wang, J.Fu, J.-N.
Zong, W.
Smith, M.C.
De Cat, P.
Shi, J.
Luo, A.
Zhang, H.
Frasca, A.
Corbally, C.J.
Molenda-Żakowicz, J.
Catanzaro, G.
Gray, R.O.
Wang, J.
Pan, Y.
Affiliation
Steward Observatory, University of ArizonaIssue Date
2020
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IOP Publishing LtdCitation
Wang, J., Fu, J. N., Zong, W., Smith, M. C., De Cat, P., Shi, J., ... & Pan, Y. (2020). LAMOST Observations in 15 K2 Campaigns. I. Low-resolution Spectra from LAMOST DR6. The Astrophysical Journal Supplement Series, 251(2), 27.Rights
Copyright © 2020. The American Astronomical Society.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
The Large Sky Area Multi-object Fiber Spectroscopic Telescope (LAMOST)-K2 (LK2) project, initiated in 2015, aims to collect low-resolution spectra of targets in the K2 campaigns, similar to the LAMOST-Kepler project. By the end of 2018, a total of 126 LK2 plates had been observed by LAMOST. After cross-matching the catalog of the LAMOST data release 6 (DR6) with that of the K2 approved targets, we found 160,619 usable spectra of 84,012 objects, most of which had been observed more than once. The effective temperature, surface gravity, metallicity, and radial velocity from 129,974 spectra for 70,895 objects are derived through the LAMOST Stellar Parameter Pipeline (LASP). The internal uncertainties were estimated to be 81 K, 0.15 dex, 0.09 dex, and 5 km s-1, respectively, when derived from a spectrum with a signal-to-noise ratio in the g band (S/N g ) of 10. These estimates are based on results for targets with multiple visits. The external accuracies were assessed by comparing the parameters of targets in common with the APOGEE and Gaia surveys, for which we generally found linear relationships. A final calibration is provided, combining external and internal uncertainties for giants and dwarfs, separately. We foresee that these spectroscopic data will be used widely in different research fields, especially in combination with K2 photometry. © 2020. The American Astronomical Society. All rights reserved.Note
Immediate accessISSN
0067-0049Version
Final published versionae974a485f413a2113503eed53cd6c53
10.3847/1538-4365/abc1ed