A visible/infra-red low noise, fast readout wavefront sensor for all-sky adaptive optics

2006 ◽  
Author(s):  
Matthew A. Kenworthy ◽  
Philip M. Hinz ◽  
Suresh Sivanandam ◽  
Andrew H. Breuninger ◽  
Frank J. Low
Keyword(s):  
Adaptive Optics ◽  
Low Noise ◽  
Wavefront Sensor ◽  
Infra Red

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

scholarly journals OCAM2S: an integral shutter ultrafast and low noise wavefront sensor camera for laser guide stars adaptive optics systems

2014 ◽  
Author(s):  
Jean-Luc Gach ◽  
Philippe Feautrier ◽  
Philippe Balard ◽  
Christian Guillaume ◽  
Eric Stadler
Keyword(s):  
Adaptive Optics ◽  
Low Noise ◽  
Wavefront Sensor ◽  
Laser Guide Stars ◽  
Laser Guide

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.

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

Low-noise adaptive optics for gravitational wave interferometers

2006 ◽  
Vol 23 (20) ◽  
pp. 5919-5925
Author(s):  
S Avino ◽  
E Calloni ◽  
A Tierno ◽  
B Agrawal ◽  
R De Rosa ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Adaptive Optics ◽  
Low Noise

Evaluating the Fraction of Obscured Supernovæ in Luminous Infrared Galaxies with Adaptive Optics Surveys

2017 ◽  
Vol 14 (S339) ◽  
pp. 335-335
Author(s):  
T. Reynolds ◽  
S. Mattila ◽  
E. Kool ◽  
E. Kankare ◽  
S. Ryder ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Detection Efficiency ◽  
Significant Proportion ◽  
Infrared Galaxies ◽  
Luminous Infrared Galaxies ◽  
Infra Red ◽  
Nuclear Background ◽  
Red Galaxies ◽  
Optical Surveys

AbstractDespite the expectation of a high supernova rate in luminous infra-red galaxies (LIRGs), a deficit has been discovered in optical surveys that is due to high levels of extinction by dust and to issues of contrast against the bright nuclear background. Searching in the near infra-red enables observations to penetrate that dust, while using adaptive-optics achieves the resolution required to observe supernovæ close to the nuclei of those galaxies. Over the last decade multiple observing programmes using the best AO instrumentation mounted on large telscopes have accumulated a dataset of many LIRGs, and met with much greater success in discovering nuclear supernovæ. However, a significant proportion is still being missed. By using techniques to evaluate our detection efficiency in these data, and simulations of the supernovæ occuring in the galaxies, we can evaluate the nature of these transients.

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