scholarly journals Simple broadband implementation of a phase contrast wavefront sensor for adaptive optics

2004 ◽  
Vol 12 (25) ◽  
pp. 6240 ◽  
Author(s):  
E. E. Bloemhof ◽  
J. K. Wallace
Keyword(s):  
Adaptive Optics ◽  
Phase Contrast ◽  
Wavefront Sensor

scholarly journals Comparison of wavefront sensor models for simulation of adaptive optics

2009 ◽  
Vol 17 (22) ◽  
pp. 20575 ◽  
Author(s):  
Zhiwen Wu ◽  
Anita Enmark ◽  
Mette Owner-Petersen ◽  
Torben Andersen
Keyword(s):  
Adaptive Optics ◽  
Wavefront Sensor ◽  
Sensor Models

scholarly journals On-sky correction of non-common path aberration with the pyramid wavefront sensor

2020 ◽  
Vol 636 ◽  
pp. A88 ◽  
Author(s):  
S. Esposito ◽  
A. Puglisi ◽  
E. Pinna ◽  
G. Agapito ◽  
F. Quirós-Pacheco ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Critical Issue ◽  
Wavefront Sensor ◽  
Interaction Matrix ◽  
Scientific Instrument ◽  
Wavefront Sensors ◽  
Successful Operation ◽  
Optical Elements ◽  
Common Path ◽  
External Conditions

The paper deals with with the on-sky performance of the pyramid wavefront sensor-based Adaptive Optics (AO) systems. These wavefront sensors are of great importance, being used in all first light AO systems of the ELTs (E-ELT, GMT, and TMT), currently in design phase. In particular, non-common path aberrations (NCPAs) are a critical issue encountered when using an AO system to produce corrected images in an associated astronomical instrument. The AO wavefront sensor (WFS) and the supported scientific instrument typically use a series of different optical elements, thus experiencing different aberrations. The usual way to correct for such NCPAs is to introduce a static offset in the WFS signals. In this way, when the AO loop is closed the sensor offsets are zeroed and the deformable mirror converges to the shape required to null the NCPA. The method assumes that the WFS operation is linear and completely described by some pre-calibrated interaction matrix. This is not the case for some frequently used wavefront sensors like the Pyramid sensor or a quad-cell Shack-Hartmann sensor. Here we present a method to work in closed-loop with a pyramid wavefront sensor, or more generally a non-linear WFS, introducing a wavefront offset that remains stable when AO correction quality changes due to variations in external conditions like star brightness, seeing, and wind speed. The paper details the methods with analytical and numerical considerations. Then we present results of tests executed at the LBT telescope, in daytime and on sky, using the FLAO system and LUCI2 facility instrument. The on-sky results clearly show the successful operation of the method that completely nulls NCPA, recovering diffraction-limited images with about 70% Strehl ratio in H band in variable seeing conditions. The proposed method is suitable for application to the above-mentioned ELT AO systems.

Very low noise Shack-Hartmann wavefront sensor for adaptive optics in the near-IR

2014 ◽  
Author(s):  
Silvère Gousset ◽  
Clélia Robert ◽  
Thierry Fusco ◽  
Vincent Michau ◽  
Cyril Petit ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Low Noise ◽  
Wavefront Sensor ◽  
Near Ir

Laboratory characterization of a Foucault-like wavefront sensor for adaptive optics

1998 ◽  
Author(s):  
Armando Riccardi ◽  
N. Bindi ◽  
Roberto Ragazzoni ◽  
Simone Esposito ◽  
Paolo Stefanini
Keyword(s):  
Adaptive Optics ◽  
Wavefront Sensor ◽  
Laboratory Characterization

Adaptive optics with advanced phase-contrast techniques II High-resolution wave-front control

2001 ◽  
Vol 18 (6) ◽  
pp. 1300 ◽  
Author(s):  
Eric W. Justh ◽  
Mikhail A. Vorontsov ◽  
Gary W. Carhart ◽  
Leonid A. Beresnev ◽  
P. S. Krishnaprasad
Keyword(s):  
High Resolution ◽  
Wave Front ◽  
Adaptive Optics ◽  
Phase Contrast ◽  
Advanced Phase
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