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    Closed-loop focal plane wavefront control with the SCExAO instrument

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    Author
    Martinache, Frantz
    Jovanovic, Nemanja
    Guyon, Olivier
    Affiliation
    Univ Arizona, Steward Observ
    Univ Arizona, Coll Opt Sci
    Issue Date
    2016-09-06
    Keywords
    instrumentation: adaptive optics
    methods: data analysis
    techniques: high angular resolution
    techniques: interferometric
    
    Metadata
    Show full item record
    Publisher
    EDP SCIENCES S A
    Citation
    Closed-loop focal plane wavefront control with the SCExAO instrument 2016, 593:A33 Astronomy & Astrophysics
    Journal
    Astronomy & Astrophysics
    Rights
    © ESO, 2016.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    Aims. This article describes the implementation of a focal plane based wavefront control loop on the high-contrast imaging instrument SCExAO (Subaru Coronagraphic Extreme Adaptive Optics). The sensor relies on the Fourier analysis of conventional focal-plane images acquired after an asymmetric mask is introduced in the pupil of the instrument. Methods. This absolute sensor is used here in a closed-loop to compensate for the non-common path errors that normally affects any imaging system relying on an upstream adaptive optics system. This specific implementation was used to control low-order modes corresponding to eight zernike modes (from focus to spherical). Results. This loop was successfully run on-sky at the Subaru Telescope and is used to offset the SCExAO deformable mirror shape used as a zero-point by the high-order wavefront sensor. The paper details the range of errors this wavefront-sensing approach can operate within and explores the impact of saturation of the data and how it can be bypassed, at a cost in performance. Conclusions. Beyond this application, because of its low hardware impact, the asymmetric pupil Fourier wavefront sensor (APF-WFS) can easily be ported in a wide variety of wavefront sensing contexts, for ground-as well space-borne telescopes, and for telescope pupils that can be continuous, segmented or even sparse. The technique is powerful because it measures the wavefront where it really matters, at the level of the science detector.
    Note
    Open Access Journal.
    ISSN
    0004-6361
    1432-0746
    DOI
    10.1051/0004-6361/201628496
    Version
    Final published version
    Additional Links
    http://www.aanda.org/10.1051/0004-6361/201628496
    ae974a485f413a2113503eed53cd6c53
    10.1051/0004-6361/201628496
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