A method of measuring the [α/Fe] ratios from the spectra of the LAMOST survey

作     者：Ji Li Chen Han Mao-Sheng Xiang Jian-Rong Shi Jing-Kun Zhao Xiao-Wei Liu Hua-Wei Zhang Hai-Bo Yuan Xuan Ci Xiao-Feng Zhang Yue-Xiang Wang Yang Huang Yong Zhang Yong-Hui Hou Yue-Fei Wang Zi-Huang Cao 

作者机构：Department of Space Science and Astronomy Hebei Normal University Shijiazhuang 050024 China Department of Astronomy Peking University Beijing 100871 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing 100871 China Department of Astronomy Beijing Normal University Beijing 100875 China Nanjing Institute of Astronomical Optics & Technology National Astronomical Observatories Chinese Academy of Sciences Nanjing 210042 China 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2016年第16卷第7期

页      面：83-96页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：supported by the National Key Basic Research Program of China(973Program,No.2014CB845700) the National Natural Science Foundation of China(Grant Nos.U1331120,U1431106,U1531118,U1531244 and 11473001) The Guo Shou Jing Telescope(the Large Sky Area MultiObject Fiber Spectroscopic Telescope,LAMOST)is aNational Major Scientific Project built by the Chinese Academy of Sciences provided by the National Development and Reform Commission.LAMOST is operated and managed by National Astronomical Observatories,Chinese Academy of Sciences 

主　　题：Galaxy evolution stars abundances stars fundamental parameters techniques spectroscopy surveys methods data analysis 

摘      要：The [α/Fe] ratios in stars are good tracers to probe the formation history of stellar populations and the chemical evolution of the Galaxy. The spectroscopic survey of LAMOST provides a good opportunity to determine [α/Fe] of millions of stars in the Galaxy. We present a method of measuring the [α/Fe]ratios from LAMOST spectra using the template-matching technique of the LSP3 pipeline. We use three test samples of stars selected from the ELODIE and MILES libraries, as well as the LEGUE survey to validate our method. Based on the test results, we conclude that our method is valid for measuring [α/Fe]from low-resolution spectra acquired by the LAMOST survey. Within the range of the stellar parameters Teff= [5000, 7500] K, log g = [1.0, 5.0] dex and [Fe/H]= [onsistent with values derived from high-resolution spectra,-1.5, ＋0.5] dex, our [α/Fe] measurements are c and the accuracy of our [α/Fe] measurements from LAMOST spectra is better than 0.1 dex with spectral signal-to-noise higher than 20.