Quantitative simulation of image correction for astronomy with a segmented active mirror.
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Correction by active mirror systems of image distortion due to atmospheric turbulence promises to improve the quality of ground-based astronomical observations. Although the ideal of fully correcting average-to-poor seeing to the diffraction limit of a large telescope cannot be easily realized with current technology, it has been demonstrated that partial correction of severe seeing disturbances can significantly improve image resolution. This paper describes a computer simulation of partial seeing correction by the Lockheed Active Mirror. Quantitative evaluation of the effects of partial correction on simulated wavefronts indicates that, even with a modest number of mirror actuators, one can achieve a diffraction-limited image superimposed on a background of scattered light.
[1] R. Hudgin. Wave-front compensation error due to finite corrector-element size , 1977 .
[2] R. Noll. Zernike polynomials and atmospheric turbulence , 1976 .
[3] David L. Fried,et al. Statistics of a Geometric Representation of Wavefront Distortion: Errata , 1965 .
[4] P. B. Ulrich,et al. Thermal blooming in the atmosphere , 1978 .
[5] Ted Tarbell,et al. a Simple Image Motion Compensation System for Solar Observations , 1980 .