FN Archimer Export Format
PT J
TI Three-sided pyramid wavefront sensor, part 1: simulations and analysis for astronomical adaptive optics
BT 
AF Schatz, Lauren
   Males, Jared R.
   Correia, Carlos
   Neichel, Benoit
   Chambouleyron, Vincent
   Codona, Johanan
   Fauvarque, Olivier
   Sauvage, Jean-François
   Fusco, Thierry
   Hart, Michael
   Janin-Potiron, Pierre
   Johnson, Robert
   Long, Joseph D.
   Mateen, Mala
AS 1:1;2:2;3:3;4:3;5:3;6:4;7:5;8:3;9:3;10:4;11:3;12:6;13:2;14:6;
FF 1:;2:;3:;4:;5:;6:;7:PDG-REM-RDT-LDCM;8:;9:;10:;11:;12:;13:;14:;
C1 University of Arizona, Wyant College of Optical Sciences, Tucson, Arizona, USA
   University of Arizona, Steward Observatory, Tucson, Arizona, USA
   Aix Marseille University, CNRS, CNES, LAM, Marseille, France
   Hart Scientific Consulting International LLC, Tucson, Arizona, USA
   IFREMER, Laboratoire Detection, Capteurs et Mesures, Plouzane, France
   Air Force Research Laboratory, Starfire Optical Range, Kirtland Air Force Base, New Mexico
C2 UNIV ARIZONA, USA
   UNIV ARIZONA, USA
   UNIV AIX MARSEILLE, FRANCE
   HART SCIENTIFIC CONSULTING INTERNATIONAL LLC, USA
   IFREMER, FRANCE
   STARFIRE OPTICAL RANGE, MEXICO
SI BREST
SE PDG-REM-RDT-LDCM
IN WOS Ifremer UPR
   copubli-france
   copubli-univ-france
   copubli-int-hors-europe
   copubli-sud
IF 1.911
TC 8
UR https://archimer.ifremer.fr/doc/00747/85864/91144.pdf
LA English
DT Article
DE ;adaptive optics;wavefront sensing;instrumentation;high contrast imaging;simulation
AB The Giant Segmented Mirror Telescopes (GSMTs) including the Giant Magellan Telescope (GMT), the Thirty Meter Telescope (TMT), and the European Extremely Large Telescope (E-ELT), all have extreme adaptive optics (ExAO) instruments planned that will use pyramid wavefront sensors (PWFS). The ExAO instruments all have common features: a high-actuator-count deformable mirror running at extreme speeds (>1  kHz); a high-performance wavefront sensor (WFS); and a high-contrast coronagraph. ExAO WFS performance is currently limited by the need for high spatial sampling of the wavefront which requires large detectors. For ExAO instruments for the next generation of telescopes, alternative architectures of WFS are under consideration because there is a trade-off between detector size, speed, and noise that reduces the performance of GSMT-ExAO wavefront control. One option under consideration for a GSMT-ExAO wavefront sensor is a three-sided PWFS (3PWFS). The 3PWFS creates three copies of the telescope pupil for wavefront sensing, compared to the conventional four-sided PWFS (4PWFS), which uses four pupils. The 3PWFS uses fewer detector pixels than the 4PWFS and should therefore be less sensitive to read noise. Here we develop a mathematical formalism based on the diffraction theory description of the Foucault knife-edge test that predicts the intensity pattern after the PWFS. Our formalism allows us to calculate the intensity in the pupil images formed by the PWFS in the presence of phase errors corresponding to arbitrary Fourier modes. We use these results to motivate how we process signals from a 3PWFS. We compare the raw intensity (RI) method, and derive the Slopes Maps (SM) calculation for the 3PWFS, which combines the three pupil images of the 3PWFS to obtain the X and Y slopes of the wavefront. We then use the Object Oriented MATLAB Adaptive Optics toolbox (OOMAO) to simulate an end-to-end model of an AO system using a PWFS with modulation and compare the performance of the 3PWFS to the 4PWFS. In the case of a low read noise detector, the Strehl ratios of the 3PWFS and 4PWFS are within 0.01. When we included higher read noise in the simulation, we found a Strehl ratio gain of 0.036 for the 3PWFS using RI over the 4PWFS using SM at a stellar magnitude of 10. At the same magnitude, the 4PWFS RI also outperformed the 4PWFS SM, but the gain was only 0.012 Strehl. This is significant because 4PWFS using SM is how the PWFS is conventionally used for AO wavefront sensing. We have found that the 3PWFS is a viable WFS that can fully reconstruct a wavefront and produce a stable closed-loop with correction comparable to that of a 4PWFS, with modestly better performance for high read-noise detectors. 
PY 2021
PD OCT
SO Journal Of Astronomical Telescopes Instruments And Systems
SN 2329-4124
PU SPIE-Intl Soc Optical Eng
VL 7
IS 4
UT 000750890500012
DI 10.1117/1.JATIS.7.4.049001
ID 85864
ER

EF