在本研究中，我们进行了模拟，以找出由于运动导致的Chinese Space Station Telescope (CSST)的Main Survey Camera (MSC)所拍摄图像的预期几何像差。正如先前工作所预期的，我们的发现表明，光的几何畸变会影响焦面的视在比例尺，并且随着焦面尺寸的增加，这种影响变得更加显著。我们的模型表明，该效应在垂直和平行方向上始终影响像素比例尺。在一个轨道周期内，视在比例尺变化呈正弦分布。模拟显示，该效应在银河系中心尤为显著，并沿黄纬方向逐渐减弱。在低黄纬处，视场边缘的总像差分别导致约0.94像素的偏移（20分钟曝光）和0.26像素的偏移（300秒曝光）。我们提出了在CSST观测前后阶段对几何效应的适当处理方法。
英文摘要：
In this study, we conducted simulations to find the geometric aberrations expected for images taken by the Main Survey Camera (MSC) of the Chinese Space Station Telescope (CSST) due to its motion. As anticipated by previous work, our findings indicate that the geometric distortion of light impacts the focal plane's apparent scale, with a more pronounced influence as the size of the focal plane increases. Our models suggest that the effect consistently influences the pixel scale in both the vertical and parallel directions. The apparent scale variation follows a sinusoidal distribution throughout one orbit period. Simulations reveal that the effect is particularly pronounced in the center of the Galaxy and gradually diminishes along the direction of ecliptic latitude. At low ecliptic latitudes, the total aberration leads to about 0.94 pixels offset (a 20-minute exposure) and 0.26 pixels offset (a 300-second exposure) at the edge of the field of view, respectively. Appropriate processings for the geometric effect during the CSST pre- and post-observation phases are presented.
Characterization of the CSST Survey Camera CCDs: I. basic electro-optical performance
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Peking University（北京大学）
A Robust Geometric Distortion Solution for Main Survey Camera of CSST
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Institute for Frontiers in Astronomy and Astrophysics of Beijing Normal University（北京师范大学前沿天文与天体物理研究所）；Zhejiang Lab（浙江实验室）；Changchun Institute of Optics, Fine Mechanics and Physics, Chinese Academy of Sciences（中国科学院长春光学精密机械与物理研究所）
Predicting the detection yields of giant planets and brown dwarfs with CSST astrometry
Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交大李政道研究所）；School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；School of Astronomy and Space Sciences, University of Chinese Academy of Sciences (UCAS)（中国科学院大学天文学与空间科学学院）；School of Physics and optoelectronic engineering, Anhui University（安徽大学物理与光电工程学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
Mock Observations for the CSST Mission: CPI-C -- Instrument Simulation
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；School of Physics and Astronomy, Sun Yat-sen University（中山大学物理与天文学院）；Center of CSST in the great bay area, Sun Yat-sen University（中山大学粤港澳大湾区CSST中心）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）
Mock Observations of Multiple Stellar Populations in Tidal Streams of Palomar 5 for the Chinese Space Station Survey Telescope
School of Physics and Astronomy, Sun Yat-sen University（中山大学物理学院）；CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area（中国空间站巡天望远镜粤港澳大湾区科学中心）
Mock Observations for the CSST Mission: Main Surveys--An Overview of Framework and Simulation Suite
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Hunan Normal University（湖南师范大学）；Yunnan University（云南大学）；Changchun Institute of Optics, Fine Mechanics and Physics, Chinese Academy of Sciences（中国科学院长春光学精密机械与物理研究所）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Beijing Normal University（北京师范大学）；Anhui University（安徽大学）
A Statistical Framework for Utilization of Simultaneous Pupil Plane and Focal Plane Telemetry for Exoplanet Imaging, Part II: The Science Camera Image as a Function of the Wavefront Sensor Field
A Statistical Framework for the Utilization of Simultaneous Pupil Plane and Focal Plane Telemetry for Exoplanet Imaging, Part I: Accounting for Aberrations in Multiple Planes
Optical Design of OPTICAM-ARG: A Three-Channel High-Time-Resolution Camera for the Jorge Sahade Telescope
Instituto de Astronomía, Universidad Nacional Autónoma de México（墨西哥国立自治大学天文学研究所）；School of Physics and Astronomy, University of Southampton（南安普顿大学物理与天文学院）；Complejo Astronómico El Leoncito (CASLEO), CONICET-UNLP-UNC-UNSJ（埃尔莱昂西托天文综合体 (CASLEO)，阿根廷国家科学技术研究委员会-拉普拉塔国立大学-科尔多瓦国立大学-圣胡安国立大学）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata（拉普拉塔国立大学天文与地球物理科学学院）
Freezing the speckles: focal plane wavefront sensing with the spatially-clipped self-coherent camera
James C. Wyant College of Optical Sciences, University of Arizona（亚利桑那大学光学科学学院）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Leiden University, Leiden Observatory（莱顿大学莱登天文台）；Flatiron Center for Computational Astrophysics, Flatiron Institute（平顶山研究所计算天体物理中心）；Starfire Optical Range, Kirtland Air Force Base（基尔兰空军基地星光光学试验场）；Northrop Grumman（诺斯罗普·格鲁曼公司）
Digging dark holes on-sky with the Self-Coherent Camera: Preliminary results
Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；Steward Observatory, The University of Arizona（斯图德天文台，亚利桑那大学）；Wyant College of Optical Sciences, The University of Arizona（怀雅特光学科学学院，亚利桑那大学）；Subaru Telescope, National Observatory of Japan, National Institutes of Natural Sciences（昴星团望远镜，日本国立天文台，日本自然科学研究院）；Astrobiology Center, National Institutes of Natural Sciences（天体生物学中心，日本自然科学研究院）；Northrop Grumman Corporation（诺斯罗普·格鲁曼公司）；Center for Computational Astrophysics, Flatiron Institute（计算天体物理学中心，富尔顿研究所）；Draper Laboratory（德拉珀实验室）；Starfire Optical Range, Kirtland Air Force Base（星光光学靶场，柯克兰空军基地）
