载人航天工程巡天空间望远镜大视场多色成像与无缝光谱巡天  

The wide-field multiband imaging and slitless spectroscopy survey to be carried out by the Survey Space Telescope of China Manned Space Program

作　　者：詹虎[1,2] Hu Zhan(National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China;Kavli Institute for Astronomy and Astrophysics,Peking University,Beijing 100871,China)

机构地区：[1]中国科学院国家天文台,北京100101 [2]北京大学科维理天文与天体物理研究所,北京100871

出　　处：《科学通报》2021年第11期1290-1298,共9页Chinese Science Bulletin

基　　金：国家自然科学基金(11033005);中国科学院战略性先导科技专项空间科学预先研究项目(XDA04070800);中国科学院天文台站设备更新及重大仪器设备运行专项、中国科学院事业单位修缮购置专项、中国科学院空间科学研究院培育项目;国家天文台预研项目和天文联合基金(U1931208)资助。

摘　　要：近20年来,以Sloan Digital Sky Survey(SDSS)[1]为代表的巡天项目取得了令人瞩目的成果,打开了用天文观测精确检验和探索基础物理理论的新篇章,催生了Vera Rubin Observatory(VRO,原名Large Synoptic Survey Telescope)、Dark Energy Spectroscopic Instrument(DESI)、Euclid、Roman Space Telescope(RST,原名Wide Field Infrared Survey Telescope)等新一代大型巡天项目.The 2 m-aperture Survey Space Telescope(also known as the China Space Station Telescope, CSST) is a major science project of China Manned Space Program. It is expected to start science operations around 2024 and has a nominal mission lifetime of 10 years. During observations, CSST will fly independently in the same orbit as the space station while maintaining a large distance apart. It can dock with the space station for refueling and servicing as scheduled or as needed.With a Cook-type three-mirror anastigmat design, CSST can achieve superior image quality within a large field of view(Fo V), which gives it an advantage for survey observations. Being an off-axis telescope without any obstruction, its point spread function(PSF) is not affected by diffraction of mirror support structures and is thus helpful for weak-lensing shear measurements. The radius encircling 80% energy of the PSF within CSST’s central 1.1 square degrees of Fo V is required to be no more than 0.15″, including all wavefront errors in the optics and instruments and dynamical effects such as the telescope’s attitude control and vibration.CSSTwill be launched with 5 first-generation instruments including a survey camera, a terahertz receiver, a multichannel imager, an integral field spectrograph, and a cool planet imaging coronagraph. The survey camera is equipped with 309 k×9 k detectors for science observations, each with a filter or grating mounted above, a defocused 9 k×9 k detector for flux calibration in r band, 8 640×512 near-infrared detectors, fine guide sensors, and wavefront sensors. The primary task of CSST is to carry out a high-resolution large-area multiband imaging and slitless spectroscopy survey covering the wavelength range of 255–1000 nm. Precision cosmology is the main science driver of the survey, and, therefore, the main area of sky selected for observation is at median-to-high galactic latitude and median-to-high ecliptic latitude. It will take the survey camera roughly 7 years of operation accumulated over 10 y

关 键 词：空间望远镜 物理理论 载人航天工程 精确检验 天文观测 光谱巡天 

分 类 号：V52[航空宇航科学与技术—人机与环境工程] P111[天文地球—天文学]