A reflective Shack-Hartmann wave-front sensor for adaptive optics

Details A reflective Shack-Hartmann wave-front sensor for adaptive optics A reflective Shack-Hartmann wave-front sensor for adaptive optics

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasp..106.1104c&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 106, no. 704, p. 1104-1110

Physics

Optics

5

Adaptive Optics, Atmospheric Optics, Imaging Techniques, Instrument Compensation, Wave Front Deformation, Wave Front Reconstruction, Wave Fronts, Atmospheric Correction, Atmospheric Effects, Atmospheric Turbulence, Near Infrared Radiation, Seeing (Astronomy)

Scientific paper

We describe a new wave-front sensor based on the efficient Shack-Hartmann quad cell system. The key improvement to existing designs is a modified lenslet array. The traditional refractive lenslet array is replaced with a segmented reflective system that allows individual control of each subaperture. This system has produced diffraction-limited slope correction of the six 1.83-m mirrors of the Multiple Mirror Telescope (MMT) using a 9.9 V magnitude guide star and significant image improvement on guide stars as faint as 11.3 V magnitude, limited by the readout noise of the CCD quad cell detector. Recent experiments with an improved detector indicate diffraction-limited imaging on guide stars as faint as the 15th magnitude. This optimized wave-front sensor, equally applicable to filled-aperture telescopes, promises to extend the amount of sky coverage available for adaptive correction in the near IR.

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