Wavefront sensing deconvolution and adaptive optics

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Abstract
For large telescopes, the fundamental limit set by the diffraction to the angular resolution can be reached if the aberrations are perfectly corrected. Two solutions are practicable: image restoration by numerical processing or real time correction by adaptive optics. These two processes require the determination of the wavefront or of the optical transfer function. New large detectors arrays can be used in wavefront sensing which then allow the measurement of the wavefront at a large number of point. The general lay-out of such an instrument is given and its accuracy evaluated. The wavefront sensing contribution to numerical image processing is studied mainly for the case of degradation by atmospheric turbulence. The improvement of numerical processing by a partial active correction is discussed.

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