天体多帧盲反卷积与天文成像PSF恢复

J. Christou, E. Hege, S. Jefferies
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引用次数: 0

摘要

天文物体的地面成像通常需要某种形式的后处理来实现记录图像中的全部信息内容。所记录的图像可以表示为:这是无噪声情况下非相干成像的标准表达式。i(r→)为测量目标,o(r→)为真实物体分布,p(r→)为光学系统的点扩散函数(PSF), *为卷积运算。因此,当已知PSF时,该表达式的反转将得到对象分布。然而,在许多情况下,PSF要么不确定,要么未知。因此,标准反褶积技术不能应用。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Multiframe Blind Deconvolution for Object and PSF Recovery for Astronomical Imaging
Ground-based imaging of astronomical objects typically requires some form of post-processing to realize the full information content in the recorded image. The recorded image can be expressed as which is the standard expression for incoherent imaging in the absence of noise. i(r→) is the measured target, o(r→) is the true object distribution, p(r→) represents the point spread function (PSF) of the optical system, and * denotes the convolution operation. Thus, when the PSF is known, inversion of this expression will yield the object distribution. However, in many cases, the PSF is either poorly determined or unknown. Thus standard deconvolution techniques cannot be applied.
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