Quality and reliability of our Shack-Hartmann wavefront sensors 

Factors important for accuracy in our Shack-Hartmann sensors

• Focal length of lenslet array : in our instruments we use long focal length for the Shack-Hartmann lenslet array (22 mm or 41 mm). Why a long focal length lenslet array is so important?
• Calibration: we can calibrate the effect of any extra optical element in your test setup
• Centroiding: very sophisticated algorithm tuned on our lenslet arrays. It also takes into account for local non-uniform illumination
• Combination of reference and test spots: our proprietary algorithm is very reliable and works in presence of very high aberrations
• Choice among 4 set of polynomials to fit to data: Annular, Standard and Fringe Zernikes and Seidel polynomials. Annular Zernikes are required when analyzing astronomical telescopes
• 70 Zernike terms: low order and higher order aberration terms for Spherical aberrations, Astigmatism, Coma etc.
• Wavefront reconstruction: independent from the Zernike aberrations, very sophisticated algorithm for integration from residuals
• As good as interferometer
• A full set of accessories (Calibration units, Beam-Expanders and Beam-Compressors) to complete your setup.
• Calibration tools for very accurate measurements: a new calibration is required whenever you insert an extra optical elements in your setup (like collimators, Beam-Expander etc.) and/or in presence of temperature variations (the standard Shack-Hartmann camera itself has temperature fluctuations). For this reason, our wavefront sensors do not use pre-calibrate images but we provide you with the tools for a quick acquisition of a calibration image whenever you require it