FN Archimer Export Format
PT J
TI Three-sided pyramid wavefront sensor, part II: preliminary demonstration on the new comprehensive adaptive optics and coronagraph test instrument testbed
BT 
AF SCHATZ, Lauren
   CODONA, Johanan
   LONG, Joseph D.
   MALES, Jared R.
   PULLEN, Weslin
   LUMBRES, Jennifer
   VAN GORKOM, Kyle
   CHAMBOULEYRON, Vincent
   CLOSE, Laird M.
   CORREIA, Carlos
   FAUVARQUE, Olivier
   FUSCO, Thierry
   GUYON, Olivier
   HART, Michael
   JANIN-POTIRON, Pierre
   JOHNSON, Robert
   JOVANOVIC, Nemanja
   MATEEN, Mala
   SAUVAGE, Jean-Francois
   NEICHEL, Benoit
AS 1:1;2:2;3:3;4:3;5:2;6:1;7:3;8:4;9:3;10:4,5;11:6;12:5,8,9;13:1,10,11;14:2;15:5,6;16:12;17:13;18:14;19:5,6,9;20:5,6;
FF 1:;2:;3:;4:;5:;6:;7:;8:;9:;10:;11:PDG-REM-RDT-LDCM;12:;13:;14:;15:;16:;17:;18:;19:;20:;
C1 Wyant College of Optical Sciences, The Univ. of Arizona, United States
   Hart Scientific Consulting International LLC, United States
   Steward Observatory, The Univ. of Arizona, United States
   Aix Marseille University, CNRS, CNES, LAM, Marseille, France
   Aix-Marseille Univ, France
   Lab. d'Astrophysique de Marseille, CNRS, France
   IFREMER, France
   Univ. Paris-Saclay, France
   ONERA, France
   Steward Observatory, United States
   Subaru Telescope, NAOJ, United States
   Air Force Research Lab, United States
   Caltech, United States
   National Institute of Natural Sciences, Japan
C2 UNIV ARIZONA, USA
   HART SCI CONSULTING INT LLC, USA
   UNIV ARIZONA, USA
   UNIV AIX MARSEILLE, FRANCE
   UNIV AIX MARSEILLE, FRANCE
   CNRS, FRANCE
   IFREMER, FRANCE
   UNIV PARIS SACLAY, FRANCE
   ONERA, FRANCE
   STEWARD OBS, USA
   NAOJ, USA
   AIR FORCE RES, USA
   CALTECH, USA
   NINS, JAPAN
SI BREST
SE PDG-REM-RDT-LDCM
IN WOS Ifremer UPR
   copubli-france
   copubli-univ-france
   copubli-int-hors-europe
IF 2.3
TC 0
UR https://archimer.ifremer.fr/doc/00822/93366/100060.pdf
LA English
DT Article
DE ;adaptive optics;wavefront sensing;instrumentation;pyramid wavefront sensor;testbed
AB The next generation of giant ground and space telescopes will have the light-collecting power to detect and characterize potentially habitable terrestrial exoplanets using high-contrast imaging for the first time. This will only be achievable if the performance of the Giant Segment Mirror Telescopes (GSMTs) extreme adaptive optics (ExAO) systems are optimized to their full potential. A key component of an ExAO system is the wavefront sensor (WFS), which measures aberrations from atmospheric turbulence. A common choice in current and next-generation instruments is the pyramid wavefront sensor (PWFS). ExAO systems require high spatial and temporal sampling of wavefronts to optimize performance and, as a result, require large detectors for the WFS. We present a closed-loop testbed demonstration of a three-sided pyramid wavefront sensor (3PWFS) as an alternative to the conventional four-sided pyramid wavefront (4PWFS) sensor for GSMT-ExAO applications on the innovative comprehensive adaptive optics and coronagraph test instrument (CACTI). The 3PWFS is less sensitive to read noise than the 4PWFS because it uses fewer detector pixels. The 3PWFS has further benefits: a high-quality three-sided pyramid optic is easier to manufacture than a four-sided pyramid. We describe the design of the two components of the CACTI system, the adaptive optics simulator and the PWFS testbed that includes both a 3PWFS and 4PWFS. We detail the error budget of the CACTI system, review its operation and calibration procedures, and discuss its current status. A preliminary experiment was performed on CACTI to study the performance of the 3PWFS to the 4PWFS in varying strengths of turbulence using both the raw intensity and slopes map signal processing methods. This experiment was repeated for a modulation radius of 1.6 and 3.25 lambda / D. We found that the performance of the two wavefront sensors is comparable if modal loop gains are tuned.(c) 2022 Society of Photo-Optical Instrumentation Engineers (SPIE) 
PY 2022
PD OCT
SO Journal Of Astronomical Telescopes Instruments And Systems
SN 2329-4124
PU Spie-soc Photo-optical Instrumentation Engineers
VL 8
IS 4
UT 000914428200019
DI 10.1117/1.JATIS.8.4.049001
ID 93366
ER

EF