一种用于天文图像校正的无波前传感器尖端/倾斜去除方法

2020 35th International Conference on Image and Vision Computing New Zealand (IVCNZ) Pub Date : 2020-11-25 DOI:10.1109/IVCNZ51579.2020.9290688

P. Taghinia, Vishnu Anand Muruganandan, R. Clare, S. Weddell

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引用次数: 1

摘要

由于大气湍流的影响，地面望远镜拍摄到的天体图像会发生扭曲。传统的大气像差相位估计方法是利用波前传感器(WFS)。可变形镜通过控制系统利用这些信息来恢复图像。然而，在本文中，我们利用无波前传感器(WFSL)方法，其中没有波前传感器。考虑到大气湍流能量的最大份额包含在小口径望远镜的2轴倾斜中，我们使用WFSL专门去除这两种模式。这种方法在速度和准确性方面都是有效的。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

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A Wavefront Sensorless Tip/Tilt Removal method for Correcting Astronomical Images

Images of astronomical objects captured by ground-based telescopes are distorted due to atmospheric turbulence. The phase of the atmospheric aberration is traditionally estimated by a wavefront sensor (WFS). This information is utilised by a deformable mirror through a control system to restore the image. However, in this paper, we utilise wavefront sensorless (WFSL) methods in which the wavefront sensor is absent. Given that the largest share of atmospheric turbulence energy is contained in the 2-axial tilt for small aperture telescopes, we use WFSL to specifically remove these two modes. This method is shown to be efficient in terms of both speed and accuracy.

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2020 35th International Conference on Image and Vision Computing New Zealand (IVCNZ)

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