Basic Survey Scheduling for the Wide Field Survey Telescope(WFST)  

作　　者：Yan-Peng Chen Ji-An Jiang Wen-Tao Luo Xian-Zhong Zheng Min Fang Chao Yang Yuan-Yu Hong Zong-Fei Lü 

机构地区：[1]Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,China [2]School of Astronomy and Space Science,University of Science and Technology of China,Hefei 230026,China [3]Department of Astronomy,University of Science and Technology of China,Hefei 230026,China [4]National Astronomical Observatory of Japan,National Institutes of Natural Sciences,2-21-1 Osawa,Mitaka,Tokyo 181-8588,Japan [5]Institute of Deep Space Sciences,Deep Space Exploration Laboratory,Hefei 230026,China

出　　处：《Research in Astronomy and Astrophysics》2024年第1期59-69,共11页天文和天体物理学研究（英文版）

基　　金：supported by the National Natural Science Foundation of China (12233005, 12073078 and 12173088);the science research grants from the China Manned Space Project with NO. CMS-CSST-2021-A02, CMS-CSST-2021-A04 and CMS-CSST-2021-A07;grants from the Cyrus Chun Ying Tang Foundations。

摘　　要：Aiming at improving the survey efficiency of the Wide Field Survey Telescope, we have developed a basic scheduling strategy that takes into account the telescope characteristics, observing conditions, and weather conditions at the Lenghu site. The sky area is divided into rectangular regions, referred to as “tiles,” with a size of2°. 577 × 2°. 634 slightly smaller than the focal area of the mosaic CCDs. These tiles are continuously filled in annulars parallel to the equator. The brightness of the sky background, which varies with the moon phase and distance from the moon, plays a significant role in determining the accessible survey fields. Approximately 50connected tiles are grouped into one block for observation. To optimize the survey schedule, we perform simulations by taking into account the length of exposures, data readout, telescope slewing, and all relevant observing conditions. We utilize the Greedy Algorithm for scheduling optimization. Additionally, we propose a dedicated dithering pattern to cover the gaps between CCDs and the four corners of the mosaic CCD array, which are located outside of the 3° field of view. This dithering pattern helps to achieve relatively uniform exposure maps for the final survey outputs.

关 键 词：telescopes surveys MOON 

分 类 号：P111[天文地球—天文学]