Anti-aliasing optical method for Shack Hartmann WFSs

Glen Herriot; Jean-Pierre Véran

doi:10.1117/12.2231801

26 July 2016 Anti-aliasing optical method for Shack Hartmann WFSs

Glen Herriot, Jean-Pierre Véran

Proceedings Volume 9909, Adaptive Optics Systems V; 99091Z (2016) https://doi.org/10.1117/12.2231801
Event: SPIE Astronomical Telescopes + Instrumentation, 2016, Edinburgh, United Kingdom

Abstract

Measurement errors due to aliasing in a Shack-Hartmann WFS are typically 40% larger in variance than the fitting error of an AO system. On bright stars, aliasing is the dominant error within the control radius of the deformable mirror. Wavefront spatial frequencies beyond the WFS’ Nyquist frequency corrupt measurements below this frequency. A common misconception is to think that aliasing primarily affects the higher spatial frequency measurements. But in fact aliasing propagates to the lowest order modes, and corrupts even tip/tilt. There are many examples including the observation that the temporal power spectrum of measured tip/tilt from a WFS does not correspond to Kolmogorov theory. We propose a simple optical modification to a SH WFS (borrowed from the digital video camera industry), and present simulation results showing that the aliasing errors are reduced.

Citation Download Citation

Glen Herriot and Jean-Pierre Véran "Anti-aliasing optical method for Shack Hartmann WFSs", Proc. SPIE 9909, Adaptive Optics Systems V, 99091Z (26 July 2016); https://doi.org/10.1117/12.2231801

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