望远镜几何扭曲实测方法仿真研究

发布时间：2018-01-06 14:44

本文关键词：望远镜几何扭曲实测方法仿真研究　出处：《天文学报》2015年06期 　论文类型：期刊论文

更多相关文章： 天体测量 技术 图像处理 方法 数值模拟

【摘要】：精确求解望远镜几何扭曲效应,有利于提高望远镜的天体测量定位精度,这对天文学的诸多学科具有十分重要的意义.为此,前人发展了一种针对密集星场抖动观测并针对观测底片迭代求解几何扭曲的自校准方法,取得了较好的效果.但是,先前的工作并未对星场的密集程度或抖动方式做进一步要求,而是经验地选择较为密集的星场和较多的抖动次数进行观测.这些经验的观测方式固然能够较好地给出几何扭曲,但有时会占用较多的望远镜观测时间导致效率较低.首先介绍了上述求解望远镜几何扭曲的一般方法;通过仿真模拟,对上述方法的有效性做评估,同时对该方法要求的星场密度和抖动次数等条件做进一步优化;最后,针对实际应用中几何扭曲改正后的定位精度与视场参考星数量的关系也做了进一步的仿真和分析.
[Abstract]:It is very important for many subjects of astronomy to solve the geometric distortion effect of telescopes accurately, which is helpful to improve the accuracy of astrometry and positioning of telescopes. Previous studies have developed a self-calibration method for the jitter observation of dense star fields and iterative geometric distortion solution for the observed negatives, which has achieved good results. Previous work has made no further demands on the intensity or jitter pattern of the star field. Instead, the more dense star field and the more jitter times are selected empirically to observe. These empirical observation methods can give better geometric distortion. But sometimes it takes up a lot of telescope observation time, which results in low efficiency. Firstly, the general method to solve the geometric distortion of telescope is introduced. Through simulation, the effectiveness of the above method is evaluated, and the satellite field density and jitter times required by the method are further optimized. Finally, the relationship between the positioning accuracy and the number of reference stars in the field of view is further simulated and analyzed.
【作者单位】：中国科学院紫金山天文台;中国科学院大学;
【基金】：国家自然科学基金项目(11273066,11178006)资助
【分类号】：P111.2
【正文快照】： 1引言研究表明,不管是在太空还是地面,望远镜几何扭曲都严重影响了天体测量定位精度[1-2].因此,精确求解望远镜的几何扭曲效应,提高天体测量定位精度,促进了包括星团,太阳系天然卫星、小行星及彗星等天体运动学研究的开展[1-7].所谓几何扭曲即望远镜探测器实测的天区图像相对

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