Phase retrieval analysis of the Hobby-Eberly Telescope primary mirror segment figure error and its implication for wavefront sensing for the new wide-field upgrade

2010 ◽  
Author(s):  
Hanshin Lee ◽  
Gary J. Hill ◽  
Michael Hart
Photonics ◽  
2020 ◽  
Vol 8 (1) ◽  
pp. 3
Author(s):  
Shun Qin ◽  
Wai Kin Chan

Accurate segmented mirror wavefront sensing and control is essential for next-generation large aperture telescope system design. In this paper, a direct tip–tilt and piston error detection technique based on model-based phase retrieval with multiple defocused images is proposed for segmented mirror wavefront sensing. In our technique, the tip–tilt and piston error are represented by a basis consisting of three basic plane functions with respect to the x, y, and z axis so that they can be parameterized by the coefficients of these bases; the coefficients then are solved by a non-linear optimization method with the defocus multi-images. Simulation results show that the proposed technique is capable of measuring high dynamic range wavefront error reaching 7λ, while resulting in high detection accuracy. The algorithm is demonstrated as robust to noise by introducing phase parameterization. In comparison, the proposed tip–tilt and piston error detection approach is much easier to implement than many existing methods, which usually introduce extra sensors and devices, as it is a technique based on multiple images. These characteristics make it promising for the application of wavefront sensing and control in next-generation large aperture telescopes.


2018 ◽  
Vol 14 (S343) ◽  
pp. 59-68
Author(s):  
Željko Ivezić ◽  
Krzysztof Suberlak ◽  
Owen M. Boberg

AbstractLSST (www.lsst.org) will be a large, wide-field ground-based system designed to obtain repeated images covering the sky visible from Cerro Pachón in northern Chile. The telescope will have an 8.4m (6.5m effective) primary mirror, a 9.6 sq.deg. field of view, and a 3.2 Gigapixel camera. In a continuous observing campaign, LSST will cover the entire observable sky every three nights to a depth of V ∼ 25 per visit (using 30-second exposures and ugrizy filter set), with exquisitely accurate astrometry and photometry. Close to a half of the sky will be visited about 800 times during the nominal 10-year survey. The project is in the construction phase with first light expected in 2020 and the beginning of regular survey operations by 2022. We describe how these data will impact AGB star research and discuss how the system could be further optimized by utilizing narrow-band TiO and CN filters.


2007 ◽  
Vol 32 (11) ◽  
pp. 1584 ◽  
Author(s):  
Arun Anand ◽  
Giancarlo Pedrini ◽  
Wolfgang Osten ◽  
Percival Almoro

2008 ◽  
Author(s):  
Bing Dong ◽  
Xin Yu ◽  
Xiaofang Zhang ◽  
Baiwei Guo ◽  
Lei Zhao

2010 ◽  
Author(s):  
Siddarayappa Bikkannavar ◽  
David Redding ◽  
Joseph Green ◽  
Scott Basinger ◽  
David Cohen ◽  
...  

2011 ◽  
Vol 36 (6) ◽  
pp. 825 ◽  
Author(s):  
Oscar Azucena ◽  
Justin Crest ◽  
Shaila Kotadia ◽  
William Sullivan ◽  
Xiaodong Tao ◽  
...  

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