FN Archimer Export Format
PT J
TI Modeling noise propagation in Fourier-filtering wavefront sensing, fundamental limits and quantitative comparison
BT 
AF Chambouleyron, Vincent
   FAUVARQUE, Olivier
   Plantet, Cédric
   Sauvage, Jean-François
   Levraud, Nicolas
   Cissé, Mahawa
   Neichel, Benoît
   Fusco, Tierry
AS 1:1;2:3;3:4;4:1,2;5:1,2;6:1,2;7:1;8:1,2;
FF 1:;2:PDG-REM-RDT-LDCM;3:;4:;5:;6:;7:;8:;
C1 Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
   DOTA, ONERA, Université Paris Saclay, F-91123 Palaiseau, France
   IFREMER, Laboratoire Detection, Capteurs et Mesures (LDCM), Centre Bretagne, ZI de la Pointe du Diable, CS 10070, 29280, Plouzane, France
   INAF - Osservatorio Astronomico di Arcetri,Italy
C2 UNIV AIX MARSEILLE, FRANCE
   UNIV PARIS SACLAY, FRANCE
   IFREMER, FRANCE
   INAF, ITALY
SI BREST
SE PDG-REM-RDT-LDCM
IN WOS Ifremer UPR
   copubli-france
   copubli-europe
   copubli-univ-france
IF 6.5
TC 1
UR https://archimer.ifremer.fr/doc/00814/92600/101174.pdf
LA English
DT Article
DE ;techniques;high angular resolution;instrumentation;adaptive optics
AB Context. Adaptive optics (AO) is a technique allowing to drastically improve ground-based telescopes angular resolution. The wavefront sensor (WFS) is one of the key components of such systems, driving the fundamental performance limitations. Aims. In this paper, we focus on a specific class of WFS: the Fourier-filtering wavefront sensors (FFWFS). This class is known for its extremely high sensitivity. However, a clear and comprehensive noise propagation model for any kind of FFWFS is lacking. Methods. Considering read-out noise and photon noise, we derive a simple and comprehensive model allowing to understand how these noises propagates in the phase reconstruction in the linear framework. Results. This new noise propagation model works for any kind of FFWFS, and allows to revisit the fundamental sensitivity limit of these sensors. Furthermore, a new comparison between widely used FFWFS is held. We focus on the two main used FFWFS classes: the Zernike WFS (ZWFS) and the pyramid WFS (PWFS), bringing new understanding of their behavior. 
PY 2023
PD FEB
SO Astronomy & Astrophysics
SN 0004-6361
PU Springer
VL 670
IS A163
UT 000936919800006
DI 10.1051/0004-6361/202245351
ID 92600
ER

EF