LAMOST
The LAMOST telescope
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| Location(s) | Xinglong Station |
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| Coordinates | 40°23′44.74″N 117°34′33.1″E / 40.3957611°N 117.575861°ECoordinates: 40°23′44.74″N 117°34′33.1″E / 40.3957611°N 117.575861°E |
| Altitude | 960 m (3,150 ft) |
| Wavelength | 370–900 nm |
| Built | September 2001–October 2008[1] |
| Telescope style | Schmidt telescope with reflective corrector |
| Diameter | 4 m |
| Secondary dia. | 6 m |
| Collecting area | 18.86 m2 |
| Focal length | 20 m (f/5) |
| Mounting | Single-axis, meridian scanning |
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The Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST), also known as the Guo Shoujing Telescope after the 13th-century Chinese astronomer, is a meridian reflecting Schmidt telescope, located in Xinglong Station, Hebei Province, China. Undertaken by the Chinese Academy of Science, the telescope is planned to conduct a 5-year spectroscopic survey of 10 million Milky Way stars, as well as millions of galaxies. The project’s budget is RMB 235 million yuan.
LAMOST is configured as a reflective Schmidt telescope with adaptive optics. There are two mirrors, each made up of a number of 1.1-metre (p-p) hexagonal deformable segments. The first mirror, MA (24 segments, fitting in a 5.72×4.4 m rectangle) is a Schmidt corrector plate in a dome at ground level. The almost-flat mirror MA reflects the light to the south, up a large slanted tunnel (25° above horizontal) to the larger spherical focusing mirror MB (37 segments, fitting in a 6.67×6.09 m rectangle). This directs light to a focal plane 1.75 metres in diameter corresponding to a five-degree field of view. The focal plane is tiled with 4000 fibre-positioning units, each feeding an optical fibre which transfers light to one of sixteen 250-channel spectrographs below.
Looking at the image opposite, MB is at the top of the left-hand supporting column of the tower, MA is in the left of the two domes at the right of the image (the rightmost, grey dome is an unrelated telescope), and the spectrographs are inside the right-hand column of the tower.
Each spectrograph has two 4k×4k CCD cameras, using e2v CCD chips, with 'blue' (370–590 nm) and 'red' (570–900 nm) sides; the telescope can also be used in a higher spectral resolution mode where the range is 510–540 and 830–890 nm.
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