TY - GEN
T1 - The Subaru coronagraphic extreme AO (SCExAO) system
T2 - Techniques and Instrumentation for Detection of Exoplanets V
AU - Garrel, Vincent
AU - Guyon, Olivier
AU - Baudoz, Pierre
AU - Martinache, Frantz
AU - Stewart, Paul
AU - Lozi, Julien
AU - Groff, Tyler
PY - 2011
Y1 - 2011
N2 - The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system is an instrument designed to be inserted between the Subaru AO188 system and the infrared HiCIAO camera in order to greatly improve the contrast in the very close (less than 0.5″) neighbourhood of stars.Next to the infrared coronagraphic path, a visible scientific path, based on a EMCCD camera, has been implemented. Benefiting from both AO correction and new data processing techniques, it is a powerful tool for high angular resolution imaging and opens numerous new science opportunities. A factor 2 to 3 in Strehl ratio is obtained compared to the AO long exposure time: up to 25% Strehl in the 650nm wavelength, depending on the image processing algorithm used and the seeing conditions. The system is able to deliver diffraction limited images at 650 nm (17 mas FWHM). Our baseline image processing algorithm is based on the selection of the best signal for each spatial frequency. We demonstrate that this approach offers significantly better results than the classical select, shift and add approach (lucky imaging).
AB - The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system is an instrument designed to be inserted between the Subaru AO188 system and the infrared HiCIAO camera in order to greatly improve the contrast in the very close (less than 0.5″) neighbourhood of stars.Next to the infrared coronagraphic path, a visible scientific path, based on a EMCCD camera, has been implemented. Benefiting from both AO correction and new data processing techniques, it is a powerful tool for high angular resolution imaging and opens numerous new science opportunities. A factor 2 to 3 in Strehl ratio is obtained compared to the AO long exposure time: up to 25% Strehl in the 650nm wavelength, depending on the image processing algorithm used and the seeing conditions. The system is able to deliver diffraction limited images at 650 nm (17 mas FWHM). Our baseline image processing algorithm is based on the selection of the best signal for each spatial frequency. We demonstrate that this approach offers significantly better results than the classical select, shift and add approach (lucky imaging).
KW - adaptive optics methods
KW - data analysis techniques
KW - high angular resolution instrumentation
KW - high angular resolution techniques
KW - image processing
KW - instrumentation
UR - http://www.scopus.com/inward/record.url?scp=80053482221&partnerID=8YFLogxK
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U2 - 10.1117/12.894309
DO - 10.1117/12.894309
M3 - Conference contribution
AN - SCOPUS:80053482221
SN - 9780819487612
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Techniques and Instrumentation for Detection of Exoplanets V
Y2 - 23 August 2011 through 24 August 2011
ER -