Optical turbulence characterization at LAMOST site: observations and models

Atmospheric optical turbulence seriously limits the performance of high angular resolution instruments. An eight-night campaign of measurements was carried out at the Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST) site in 2011, to characterize the optical turbulence. Two instruments were set up during the campaign: a differential image motion monitor (DIMM) used to measure the total atmospheric seeing, and a single star Scidar (SSS) to measure the vertical profiles of the turbulence C-n(2) (h) and the horizontal wind velocity v(h). The optical turbulence parameters are also calculated with the Weather Research and Forecasting (WRF) model coupled with the Trinquet-Vernin model, which describes optical effects of atmospheric turbulence by using the local meteorological parameters. This paper presents assessment of the optical parameters involved in high angular resolution astronomy. Its includes seeing, isoplanatic angle, coherence time, coherence etendue, vertical profiles of optical turbulence intensity C-n(2) (h) and horizontal wind speed v(h). The median seeing is respectively 1.01, 1.17 and 1.07 arcsec as measured with the DIMM, the SSS and predicted with WRF model. The history of seeing measurements at the LAMOST site is reviewed, and the turbulence measurements in this campaign are compared with other astronomical observatories in the world.