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

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.

The white dwarf binary pathways survey – II. Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4

“…LAMOST is a ≃ 4 meter quasi-meridian reflecting Schmidt telescope located at Xinglong Observing Station in the Hebei province of China (Cui et al 2012). It has a field of view of 5 • in diameter and it is exclusively dedicated to obtain optical spectroscopy of celestial objects.…”

“…These were selected as F, G, K stars with northernhemisphere LAMOST (Large Sky Area Multi-Object Fibre Spectroscopic Telescope; Cui et al 2012;Zhao et al 2012) or southern-hemiesphere RAVE (Radial Velocity Experiment; Kordopatis et al 2013) spectra displaying ultraviolet (UV) excess as indicated by their GALEX (Galaxy Evolution Explorer; Martin et al 2005) FUV-NUV colours (where FUV and NUV are the far-UV and near-UV magnitudes) in a T eff vs. FUV-NUV diagram (see Figure 1). This resulted in 430 WD+FGK binary candidates from RAVE DR 1 and 504 candidates from LAMOST DR 1.…”

Spectral classification and composites of galaxies in LAMOST DR4

“…The telescope is characterized by both a large field of view and large aperture, with an effective aperture of 3.6-4.9m and 4,000 fibers mounted on its focal plane. Its spectral wavelength ranges from 3800Å to 9000Å and spectral resolution is about R∼1800 (Cui et al 2012. The fourth data release (DR4) of LAMOST includes the pilot survey(2011 October to 2012 June) and the regular survey(2012 September to 2016 June), and will be public released in June 2018.…”

HD 24355 observed by theKepler K2mission: a rapidly oscillating Ap star pulsating in a distorted quadrupole mode

“…In addition to our data, HD 24355 has been observed as part of the LAMOST campaign (Cui et al 2012;Zhao et al 2012) and was made public as part of Data Release 1 (DR1; Luo et al 2015). The LAMOST spectrum was obtained at a resolution of R ∼ 1800, and is shown in Fig.…”