000002918 001__ 2918
000002918 005__ 20160909153648.0
000002918 0247_ $$2DOI$$a10.3847/0067-0049/225/2/28
000002918 037__ $$aSCART-2016-0015
000002918 100__ $$aRen, Anbing
000002918 245__ $$aLAMOST Observations in the Kepler Field. Analysis of the Stellar Parameters Measured with LASP Based on Low-resolution Spectra
000002918 260__ $$c2016
000002918 520__ $$aAll 14 subfields of the Kepler field were observed at least once with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, Xinglong Observatory, China) during the 2012–2014 observation seasons. There are 88,628 reduced spectra with a signal-to-noise ratio in the g band (S/N_g ) ≥ 6 after the first round (2012–2014) of observations of the LAMOST– Kepler project (LK-project). By adopting the upgraded version of the LAMOST Stellar Parameter pipeline (LASP), we have determined the atmospheric parameters (T_eff, logg, and [Fe/H]) and heliocentric radial velocity v_rad for 51,406 stars with 61,226 spectra. Compared with the atmospheric parameters derived from both high-resolution spectroscopy and asteroseismology for common stars in Huber et al., an external calibration of LASP atmospheric parameters was made, leading to the determination of the external errors for giants and dwarfs. Multiple spectroscopic observations of the same objects in the LK-project were used to estimate the internal uncertainties of the atmospheric parameters as a function of S/N_g with the unbiased estimation method. The LASP atmospheric parameters were calibrated based on both the external and internal uncertainties for the giants and dwarfs. A general statistical analysis of the stellar parameters leads to the discovery of 106 candidate metal-poor stars, 9 candidate very metal-poor stars, and 18 candidate high-velocity stars. Fitting formulae were obtained segmentally for both the calibrated atmospheric parameters of the LK-project and the Kepler Input Catalog (KIC) parameters with common stars. The calibrated atmospheric parameters and radial velocities of the LK-project will be useful for studying stars in the Kepler field.
000002918 594__ $$aNO
000002918 6531_ $$aastronomical databases: miscellaneous
000002918 6531_ $$astars: fundamental parameters
000002918 6531_ $$astars: general
000002918 6531_ $$astars: statistics
000002918 700__ $$aFu, Jianning
000002918 700__ $$aDe Cat, Peter
000002918 700__ $$aWu, Yue
000002918 700__ $$aYang, Xiaohu
000002918 700__ $$aShi, Jianrong
000002918 700__ $$aLuo, Ali
000002918 700__ $$aZhang, Haotong
000002918 700__ $$aDong, Subo
000002918 700__ $$aZhang, Ruyuan
000002918 700__ $$aZhang, Yong
000002918 700__ $$aHou, Yonghui
000002918 700__ $$aWang, Yuefei
000002918 700__ $$aCao, Zihuang
000002918 700__ $$aDu, Bing
000002918 773__ $$cA28 (1-17)$$n2$$pThe Astrophysical Journal Supplement Series$$v225$$y2016
000002918 8560_ $$fpeter.decat@observatoire.be
000002918 85642 $$ahttp://iopscience.iop.org/article/10.3847/0067-0049/225/2/28/pdf
000002918 905__ $$apublished in
000002918 980__ $$aREFERD