Wavefront detector optimization for laser guided adaptive telescopes

Details Wavefront detector optimization for laser guided adaptive telescopes Wavefront detector optimization for laser guided adaptive telescopes

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989spie.1114..160k&link_type=abstract

IN: Active telescope systems; Proceedings of the Meeting, Orlando, FL, Mar. 28-31, 1989 (A90-30852 12-74). Bellingham, WA, Socie

Physics

Optics

3

Adaptive Optics, Atmospheric Correction, Laser Guidance, Telescopes, Wave Front Deformation, Accuracy, Atmospheric Turbulence, Optimization, Seeing (Astronomy)

Scientific paper

Existing instruments often use a Hartmann-Shack (H-S) wavefront sensor to conduct active measurements of the wavefront perturbations generated by atmospheric turbulence. An analysis is presently conducted of the accuracy with which a CCD array in the focal plane measures the centroid spot whose detection is rendered equivalent to the problem of phase-tilt detection by the H-S sensor's lens; attention is given to the finite pixel dimension, pixel quantity, and the superfluous space between pixels. If a telescope Strehl ratio of 0.85 is required, then on the basis of reasonable detector-parameter values a flux/seeing cell return of 115 photocounts/measurement is needed.

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