The first data release (DR1) of the LAMOST regular survey

Abstract

The Large sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) general survey is a spectroscopic survey that will eventually cover approximately half of the celestial sphere and collect 10 million spectra of stars, galaxies and QSOs. Objects in both the pilot survey and the first year regular survey are included in the LAMOST DR1. The pilot survey started in October 2011 and ended in June 2012, and the data have been released to the public as the LAMOST Pilot Data Release in August 2012. The regular survey started in September 2012, and completed its first year of operation in June 2013. The LAMOST DR1 includes a total of 1202 plates containing 2 955 336 spectra, of which 1 790 879 spectra have observed signalto-noise ratio (SNR) ≥ 10. All data with SNR ≥ 2 are formally released as LAMOST DR1 under the LAMOST data policy. This data release contains a total of 2 204 696 spectra, of which 1 944 329 are stellar spectra, 12 082 are galaxy spectra and 5017 are quasars. The DR1 not only includes spectra, but also three stellar catalogs with measured parameters: late A,FGK-type stars with high quality spectra (1 061 918 entries), A-type stars (100 073 entries), and M-type stars (121 522 entries). This paper introduces the survey design, the observational and instrumental limitations, data reduction and analysis, and some caveats. A description of the FITS structure of spectral files and parameter catalogs is also provided.

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

“…The raw spectra are reduced by the LAMOST twodimensional (2D) pipeline (Luo et al 2012(Luo et al , 2015, which extracts spectra from raw CCD images and calibrates them. This procedure includes dark and bias subtraction, cosmic ray removal, one-dimensional (1D) spectral extraction, flat-field correction, wavelength calibration, sky subtraction, merging sub-exposures and combining wavelength bands (after flux calibration).…”

Spectral classification and composites of galaxies in LAMOST DR4

“…There are two main regions of the extragalactic survey (Luo et al 2015). One is in the Northern Galactic Cap region(b ≥ 30 • ), and about 77,154 spectra are observed in this region.…”

“…However, there are some uncertainties in the shape of the continua of LAMOST spectra caused by the current method of relative flux calibration (Luo et al 2015), which may lead to an unprecise result of continuumfitting. For the current used flux calibration of LAMOST spectra, some F type dwarfs with high quality spectra are chosen as standards to get the total response curve and the reddening of the standard stars is uncertain.…”

“…With the LAMOST spectroscopic survey going on, a large data set is provided to study galaxies in our nearby universe (Luo et al 2015). Several well-known surveys have been carried out such as the Sloan Digital Sky Survey (SDSS) (York et al 2000) which observed the largest number of extragalactic targets.…”

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.…”