MAVIS: preliminary design overview of the natural guide star wavefront sensor submodule

Bonaglia, Marco; Agapito, Guido; Aliverti, Matteo; Briguglio, Runa; Busoni, Lorenzo; Capasso, Giulio; Carbonaro, Luca A.; Colapietro, Mirko; Vecchio, Ciro Del; D’Orsi, Sergio; Doniselli, Simone; Grani, Paolo; Greggio, Davide; Lapucci, Tommaso; Plantet, Cédric; Pinna, Enrico; Puglisi, Alfio; Rossi, Fábio; Savarese, Salvatore; Schipani, P.; Selmi, Chiara; Viotto, Valentina; Rigaut, François

doi:10.1117/12.2628799

Cited by 4 publications

(3 citation statements)

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“…The NIR cameras implemented in the NGS WFS design are based on the Saphira detector array. A more detailed description of the NGS WFS can be found in [15].  Laser Guide Star wavefront sensor module (LGS WFS): it is the high-order wavefront sensor of MAVIS.…”

Section: Aom Design Conceptmentioning

confidence: 99%

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MAVIS: preliminary design of the adaptive optics module

Viotto

Pinna

Agapito

et al. 2022

Adaptive Optics Systems VIII

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MAVIS will be part of the next generation of VLT instrumentation and it will include a visible imager and a spectrograph, both fed by a common Adaptive Optics Module. The AOM consists in a MCAO system, whose challenge is to provide a 30" AO-corrected FoV in the visible domain, with good performance in a 50% sky coverage at the Galactic Pole. To reach the required performance, the current AOM scheme includes the use of up to 11 reference sources at the same time ( 8LGSs + 3 NGSs) to drive more than 5000 actuators, divided into 3 deformable mirrors (one of them being UT4 secondary mirror). The system also includes some auxiliary loops, that are meant to compensate for internal instabilities (including WFSs focus signal, LGS tip-tilt signal and pupil position) so to push the stability of the main AO loop and the overall performance. Here we present the Preliminary Design of the AOM, which evolved, since the previous phase, as the result of further trade-offs and optimizations. We also introduce the main calibration strategy for the loops and sub-systems, including NCPA calibration approach. Finally, we present a summary of the main results of the performance and stability analyses performed for the current design phase, in order to show compliance to the performance requirements.

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Section: Aom Design Conceptmentioning

confidence: 99%

“…The NIR cameras implemented in the NGS WFS design are based on the Saphira detector array. A more detailed description of the NGS WFS can be found in[15].…”

mentioning

confidence: 99%

MAVIS: preliminary design of the adaptive optics module

Viotto

Pinna

Agapito

et al. 2022

Adaptive Optics Systems VIII

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“…In the framework of MAVIS, we plan to use the light from three NGSs to correct the tip-tilt (TT) and low-order errors of the wavefront. 7 Simultaneously, the instrument employs eight laser beacons, which serve the purpose of measuring and mitigating higher-order aberrations, thus ensuring comprehensive wavefront correction. 8 Another significant factor that can degrade image quality is distortions, including those induced by turbulence and optics, which are typically described as a series of polynomials of increasing degree.…”

Section: Introductionmentioning

confidence: 99%

MAVIS: optical distortions of the NGS WFS channel and their impact on the plate scale variation during tracking

Rebrysh,

Greggio,

Carlà

et al. 2024

Optical Design and Engineering IX

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Natural Guide Star (NGS) wavefront sensors (WFS) play a crucial role in multi-conjugate adaptive optics systems by detecting low-order aberrations that laser guide stars cannot measure. In the framework of MAVIS, we plan to use the light from three NGSs to correct the tip-tilt and low-order errors of the wavefront. In this work, we conduct the analysis of the distortions caused by mid-spatial frequency figure errors of the optical surfaces in the NGS WFS channel of the adaptive optics module of MAVIS. These distortions, stemming from component imperfections, can significantly impact wavefront measurements and, consequently, the plate scale in the image plane of the entire instrument. We analyse their influence on the plate scale variations during tracking. Our study quantifies the effect, shedding light on the impact of non-common path distortions between the NGS WFS and the scientific instruments on plate scale variations, ultimately contributing to optimising the MAVIS performance.

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