scholarly journals Simulation and experimental demonstration of a linearized adaptive optics control loop

2010 ◽  
Vol 7 (15) ◽  
pp. 79-79
Author(s):  
K. Li ◽  
S. Mishra ◽  
A. Roorda
Keyword(s):  
Adaptive Optics ◽  
Experimental Demonstration ◽  
Control Loop

Experimental demonstration of laser tomographic adaptive optics on a 30-meter telescope at 800 nm

2010 ◽  
Author(s):  
S, Mark Ammons ◽  
Luke Johnson ◽  
Renate Kupke ◽  
Donald T. Gavel ◽  
Claire E. Max
Keyword(s):  
Adaptive Optics ◽  
Experimental Demonstration

scholarly journals Pushing point-spread function reconstruction to the next level: application to SPHERE/ZIMPOL

2020 ◽  
Vol 494 (1) ◽  
pp. 775-788 ◽  
Author(s):  
O Beltramo-Martin ◽  
A Marasco ◽  
T Fusco ◽  
D Massari ◽  
J Milli ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Point Spread Function ◽  
Optimal Solution ◽  
Initial Guess ◽  
Control Loop ◽  
Source Characterization ◽  
Point Spread ◽  
Spread Function ◽  
Best Fitting ◽  
Established Technique

ABSTRACT Point-spread function (PSF) reconstruction (PSF-R) is a well-established technique to determine the PSF reliably and accurately from adaptive optics (AO) control-loop data. We have successfully applied this technique to improve the precision of photometry and astrometry for observations of NGC 6121 obtained with the Spectro Polarimetric High-contrast Exoplanet REsearch (SPHERE)/Zurich IMaging POLarimeter (ZIMPOL), which will be presented in a forthcoming Letter. First, we present the methodology we followed to reconstruct the PSF by combining pupil-plane and focal-plane measurements using our PSF-R method PRIME (PSF Reconstruction and Identification for Multiple-source characterization Enhancement), with upgrades of both the model and best-fitting steps compared with previous articles. Secondly, we highlight that PRIME allows us to maintain the PSF fitting residual below 0.2 per cent over 2 hours of observation and using only 30 s of AO telemetry, which may have important consequences for telemetry storage for PSF-R purposes on future 30–40 m class telescopes. Finally, we deploy PRIME in a more realistic regime using faint stars, so as to identify the precision needed on the initial-guess parameters to ensure convergence towards the optimal solution.

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