Volume 593, September 2016
|Number of page(s)||8|
|Published online||06 September 2016|
Closed-loop focal plane wavefront control with the SCExAO instrument
1 Laboratoire Lagrange, Université Côte
d’Azur, Observatoire de la Côte d’Azur, CNRS, Parc Valrose, Bât. H. Fizeau, 06108 Nice, France
2 National Astronomical Observatory of Japan, Subaru Telescope, 650 North A’Ohoku Place, Hilo, HI 96720, USA
3 Department of Physics and Astronomy, Macquarie University, 2109 Sydney, Australia
4 Steward Observatory, University of Arizona, Tucson, AZ 85721, USA
5 College of Optical Sciences, University of Arizona, Tucson, AZ 85721, USA
Accepted: 29 April 2016
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.
Key words: instrumentation: adaptive optics / methods: data analysis / techniques: high angular resolution / techniques: interferometric
© ESO, 2016
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