10 July 2008 Astronomical extended object image reconstruction after primary correction by Yunnan Observatory 1.2m adaptive optics system
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Proceedings Volume 7015, Adaptive Optics Systems; 70152D (2008); doi: 10.1117/12.787399
Event: SPIE Astronomical Telescopes + Instrumentation, 2008, Marseille, France
Abstract
As an astronomical image post-processing technique, deconvolution from wavefront sensing (DWFS) is a powerful and low cost method for adaptive optics (AO) images reduction. It is based on deconvolution of short exposure images and simultaneous measuring wavefront sensor data, both are provided by adaptive optics system to improve the quality of images. However, for extended or dim sources observing, limited precision of the Wave Front Sensor (WFS) will lead to inferior correction quality of AO images, also these can hardly enhanced by DWFS method. We show here a simple and efficient solution, which combines the DWFS method with a shift-and-add (SAA) image reconstruction technique, designed for reduction of astronomical data obtained with AO system, especially extended objects. This scheme has been applied to the upgraded 61-actuator Shack-Hartmann based adaptive optics system, partially primary corrected extended object images at Yunnan observatory 1.2m telescope for astronomical high resolution imaging. Experimental result of Mars was presented.
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Xiang Chang, Rongwang Li, Yaoheng Xiong, "Astronomical extended object image reconstruction after primary correction by Yunnan Observatory 1.2m adaptive optics system", Proc. SPIE 7015, Adaptive Optics Systems, 70152D (10 July 2008); doi: 10.1117/12.787399; https://doi.org/10.1117/12.787399
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KEYWORDS
Adaptive optics

Image restoration

Observatories

Astronomy

Wavefront sensors

Point spread functions

Optical transfer functions

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