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Wavefront sensors encode phase information of an incoming wavefront into anintensity pattern that can be measured on a camera. Several kinds of wavefrontsensors (WFS) are used in astronomical adaptive optics. Amongst them,Fourier-based wavefront sensors perform a filtering operation on the wavefrontin the focal plane. The most well known example of a WFS of this kind is theZernike wavefront sensor, and the pyramid wavefront sensor (PWFS) also belongsto this class. Based on this same principle, new WFSs can be proposed such asthe n-faced pyramid (which ultimately becomes an axicone) or the flattenedpyramid, depending on whether the image formation is incoherent or coherent. Inorder to test such novel concepts, the LOOPS adaptive optics testbed hosted atthe Laboratoire d'Astrophysique de Marseille has been upgraded by adding aSpatial Light Modulator (SLM). This device, placed in a focal plane produceshigh-definition phase masks that mimic otherwise bulk optic devices. In thispaper, we first present the optical design and upgrades made to theexperimental setup of the LOOPS bench. Then, we focus on the generation of thephase masks with the SLM and the implications of having such a device in afocal plane. Finally, we present the first closed-loop results in either staticor dynamic mode with different WFS applied on the SLM.

Adaptive optics with programmable Fourier-based wavefront sensors: a spatial light modulator approach to the LOOPS testbed