Invited Review

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST)

Xiang-Qun Cui, Yong-Heng Zhao, Yao-Quan Chu, Guo-Ping Li, Qi Li, Li-Ping Zhang, Hong-Jun Su, Zheng-Qiu Yao, Ya-Nan Wang, Xiao-Zheng Xing, Xin-Nan Li, Yong-Tian Zhu, Gang Wang, Bo-Zhong Gu, A-Li Luo, Xin-Qi Xu, Zhen-Chao Zhang, Gen-Rong Liu, Hao-Tong Zhang, De-Hua Yang, Shu-Yun Cao, Hai-Yuan Chen, Jian-Jun Chen, Kun-Xin Chen, Ying Chen, Jia-Ru Chu, Lei Feng, Xue-Fei Gong, Yong-Hui Hou, Hong-Zhuan Hu, Ning-Sheng Hu, Zhong-Wen Hu, Lei Jia, Fang-Hua Jiang, Xiang Jiang, Zi-Bo Jiang, Ge Jin, Ai-Hua Li, Yan Li, Ye-Ping Li, Guan-Qun Liu, Zhi-Gang Liu, Wen-Zhi Lu, Yin-Dun Mao, Li Men, Yong-Jun Qi, Zhao-Xiang Qi, Huo-Ming Shi, Zheng-Hong Tang, Qing-Sheng Tao, Da-Qi Wang, Dan Wang, Guo-Min Wang, Hai Wang, Jia-Ning Wang, Jian Wang, Jian-Ling Wang, Jian-Ping Wang, Lei Wang, Shu-Qing Wang, You Wang, Yue-Fei Wang, Ling-Zhe Xu, Yan Xu, Shi-Hai Yang, Yong Yu, Hui Yuan, Xiang-Yan Yuan, Chao Zhai, Jing Zha ng, Yan-Xia Zhang, Yong Zhang, Ming Zhao, Fang Zhou, Guo-Hua Zhou, Jie Zhu, Si-Cheng Zou


Abstract The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, also called the Guo Shou Jing Telescope) is a special reflecting Schmidt telescope. LAMOST’s special design allows both a large aperture (effective aperture of 3.6 m–4.9 m) and a wide field of view (FOV) (5°). It has an innovative active reflecting Schmidt configuration which continuously changes the mirror’s surface that adjusts during the observation process and combines thin deformable mirror active optics with segmented active optics. Its primary mirror (6.67 m×6.05 m) and active Schmidt mirror (5.74 m×4.40 m) are both segmented, and composed of 37 and 24 hexagonal sub-mirrors respectively. By using a parallel controllable fiber positioning technique, the focal surface of 1.75 m in diameter can accommodate 4000 optical fibers. Also, LAMOST has 16 spectrographs with 32 CCD cameras. LAMOST will be the telescope with the highest rate of spectral acquisition. As a national large scientific project, the LAMOST project was formally proposed in 1996, and approved by the Chinese government in 1997. The construction started in 2001, was completed in 2008 and passed the official acceptance in June 2009. The LAMOST pilot survey was started in October 2011 and the spectroscopic survey will launch in September 2012. Up to now, LAMOST has released more than 480 000 spectra of objects. LAMOST will make an important contribution to the study of the large-scale structure of the Universe, structure and evolution of the Galaxy, and cross-identification of multiwaveband properties in celestial objects.


Keywords techniques: wide field telescope — active optics — multi fiber — spec- troscopy survey — data reduction

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