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Adaptive optics is a technique mostly used on large telescopes. It turns outto be challenging for smaller telescopes (0.5~2m) due to the small isoplanaticangle, small subapertures and high correction speeds needed at visiblewavelengths, requiring bright stars for guiding, severely limiting the skycoverage. NGS SCAO is ideal for planetary objects but remains limited forgeneral purpose observing. The approach we consider is a compromise betweenimage quality gain and sky coverage: we propose to partially improve the imagequality anywhere in the sky instead of providing the diffraction limit around afew thousand bright stars. We suggest a new solution based on multiple AOconcepts brought together: The principle is based on a rotating Foucault test,like the first AO concept proposed by H. Babcock in 1953, on the Ground LayerAdaptive Optics, proposed by Rigaut and Tokovinin in the early 2000s, and onthe idea of Layer-oriented MCAO and the pupil-plane wavefront analysis by R.Ragazzoni. We propose to combine these techniques to use all the lightavailable in a large field to measure the ground layer turbulence and enablethe high angular resolution imaging of regions of the sky (e.g., nebulas,galaxies) inaccessible to traditional AO systems. The motivation to developcompact and robust AO system for small telescopes is two-fold: On the one hand,universities often have access to small telescopes as part of their educationprograms. Also, researchers in countries with fewer resources could alsobenefit from reliable adaptive optics system on smaller telescopes for researchand education purposes. On the other hand, amateur astronomers and enthusiastswant improved image quality for visual observation and astrophotography.Implementing readily accessible adaptive optics in astronomy clubs would alsolikely have a significant impact on citizen science.

V(WF)$^2$S: Very Wide Field WaveFront Sensor for GLAO