基于几何扭曲模型的CCD图像扭曲校正残差及分析  

Residuals and Analysis of Geometric Distortion Correction of CCD Images Based on Geometric Distortion Pattern

作　　者：傅夏青 彭青玉[1,2] 冯杰[1,2] 

机构地区：[1]暨南大学计算机科学系,广东广州510632 [2]暨南大学中法天体测量动力学与空间科学联合实验室,广东广州510632

出　　处：《天文研究与技术》2016年第3期382-388,共7页Astronomical Research & Technology

基　　金：国家自然科学基金(11273014;U1431227)资助

摘　　要：在已知图像几何扭曲模型的基础上,对2013年2月5日使用云南天文台2.4 m望远镜观测近地小行星(99942)Apophis资料中的58幅CCD图像进行了几何扭曲校正,并对校正后的图像测出的星像位置进行了几何扭曲残差分析。结果发现,星像位置X、Y两个方向的几何扭曲残差约在±0.02 pixel内。为了探究影响几何扭曲残差大小的因素,设计了仿真实验。将模拟星像函数经过设定的扭曲函数模型添加几何扭曲,得到受扭曲的星像函数,并对扭曲前后的星像进行几何扭曲残差分析。结果显示,星像的半峰全宽(FWHM)越大,几何扭曲模型的扭曲变化越快,几何扭曲残差越大。Fifty eight CCD frames taken by the 2. 4m telescope of Yunnan Observatories on Feb 5,2013 were corrected for their Geometric Distortions（ GDs） with the solved GD pattern by the approach proposed in Reference [2]. It is found that the GD residuals of the pixel position of stars still exist about ± 0. 02 pixels in both X and Y directions while they are bigger at some corners and smaller in the middle part of each CCD frame. A simulation experiment was then carried out to analyze the cause that affects the GD residuals. Our results show that the GD residuals grow bigger when the FWHM（ Full Width at Half Maximum） of a CCD stellar image becomes bigger or the GD pattern changes fast. This experiment can explain the variation of the GD residuals of stars after correcting the GDs.

关 键 词：天体测量 几何扭曲 扭曲校正 仿真 

分 类 号：P123.22[天文地球—天体测量]