Single-image wavefront curvature sensing

Details Single-image wavefront curvature sensing Single-image wavefront curvature sensing

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994spie.2201..549h&link_type=abstract

Proc. SPIE Vol. 2201, p. 549-554, Adaptive Optics in Astronomy, Mark A. Ealey; Fritz Merkle; Eds.

Physics

Optics

3

Scientific paper

A single defocused star image contains sufficient information to uniquely determine the spatial phase fluctuations of the incident wavefront. A sensor which responds to the intensity distribution in the image produces signals proportional to the wavefront curvature within the pupil and the radial slope at the pupil boundary. Unlike Roddier's differential curvature sensing technique, a single-image sensor does not cancel intensity fluctuations due to atmospheric scintillation. However, it has been shown that at typical astronomical sites the scintillation signal is negligibly small. A single-image curvature sensor can theoretically achieve a signal-to-noise ratio of order Q approximately equals r(superscript 2)(subscript 0)/(lambda) z(subscript 0) where r(subscript 0) is Fried's correlation length, (lambda) is the wavelength, and z(subscript 0) is the root-mean-square distance through the atmosphere, weighted by the refractive index structure constant C(superscript 2)(subscript n). This is more than adequate for AO systems whenever D/r(subscript 0)

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