2020/12/14 by Roberto Ragazzoni, Valentina Viotto, Ragazzoni, Roberto +25
Engineering · Physics and Astronomy · #Adaptive optics and wavefront sensing #Advanced optical system design #FOS: Physical sciences #Instrumentation and Methods for Astrophysics (astro-ph.IM) #Optical Systems and Laser Technology
paper · pdf · doi:10.48550/arxiv.2012.07560
openalex publication_date 2020/12/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The basic outline of a pupil plane WaveFront Sensor is reviewed taking into account that the source to be sensed could be different from an unresolved source, i.e. it is extended, and that it could deploy also in a 3D fashion, enough to exceed the field's depth of the observing telescope. Under these conditions it is pointed out that the features of the reference are not invariant for different position on the pupil and it is shown that the INGOT WFS is the equivalent of the Pyramid for a Laser Guide Star. Under these conditions one can imagine to use a Dark WFS approach to improve the SNR of such a WFS, or to use a corrected upward beam in order to achieve a better use of the LGS photons with respect to an ideal Shack-Hartmann WFS.