MAORY: the adaptive optics module for the Extremely Large Telescope (ELT)

Ciliegi, P.; Agapito, Guido; Aliverti, Matteo; Arcidiacono, Carmelo; Balestra, Andrea; Baruffolo, A.; Bergomi, Maria; Bianco, Andrea; Bonaglia, Marco; Busoni, Lorenzo; Cantiello, M.; Cascone, E.; Chinellato, Simonetta; Cianniello, Vincenzo; Correia, Jean-Jacques; Cosentino, Giuseppe; Caprio, Vincenzo De; Devaney, Nicholas; Antonio, Ivan Di; Cianno, A. Di; Giammatteo, Ugo Di; Rico, G. Di; Dolci, M.; Eredia, Christian; Farinato, Jacopo; Esposito, Simone; Fantinel, D.; Feautrier, Philippe; Foppiani, Italo; Giro, E.; Gluck, Laurance; Goncharov, Alexander V.; Grani, Paolo; Gullieuszik, Marco; Haguenauer, Pierre; Hénault, François; Louarn, Miska Le; Magrin, Demetrio; Malone, Deborah; Marafatto, Luca; Munari, Matteo; Oberti, Sylvain; Pariani, Giorgio; Pettazzi, Lorenzo; Plantet, Cédric; Portaluri, Elisa; Puglisi, Alfio; Rabou, Patrick; Ragazzoni, Roberto; Rakich, Andrew; Redaelli, Edoardo; Riva, M.; Rochat, S.; Rodeghiero, Gabriele; Salasnich, Bernardo; Sordo, R.; Sztefek, Marie-Helene; Valentini, Angelo; Vérinaud, Christophe; Xompero, Marco; Hubert, Z.

doi:10.1117/12.2561754

Cited by 13 publications

(8 citation statements)

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“…MAORY is the MCAO module of the ELT. 8,9 It will feed MICADO. The PSF shape also depends on the vertical structure of the atmosphere, and the magnitude / location of the required NGSs.…”

Section: Adaptive Optics For the Eltmentioning

confidence: 99%

TIPTOP: a new tool to efficiently predict your favorite AO PSF

Neichel

Beltramo-Martin

Plantet

et al. 2021

Adaptive Optics Systems VII

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The Adaptive Optics (AO) performance significantly depends on the available Natural Guide Stars (NGSs) and a wide range of atmospheric conditions (seeing, Cn2, windspeed, . . . ). In order to be able to easily predict the AO performance, we have developed a fast algorithm -called TIPTOP -producing the expected AO Point Spread Function (PSF) for any of the existing AO observing modes (SCAO, LTAO, MCAO, GLAO), and any atmospheric conditions. This TIPTOP tool takes its roots in an analytical approach, where the simulations are done in the Fourier domain. This allows to reach a very fast computation time (few seconds per PSF), and efficiently explore the wide parameter space. TIPTOP has been developed in Python, taking advantage of previous work developed in different languages, and unifying them in a single framework. The TIPTOP app is available on GitHub at: https://github.com/FabioRossiArcetri/TIPTOP, and will serve as one of the bricks for the ELT Exposure Time Calculator.

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“…MAORY is the MCAO module of the ELT. 8,9 It will feed MICADO. The PSF shape also depends on the vertical structure of the atmosphere, and the magnitude / location of the required NGSs.…”

Section: Adaptive Optics For the Eltmentioning

confidence: 99%

TIPTOP: a new tool to efficiently predict your favorite AO PSF

Neichel

Beltramo-Martin

Plantet

et al. 2021

Adaptive Optics Systems VII

Self Cite

View full text Add to dashboard Cite

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“…Despite being a forced choice for LGS sensing, the SHWFS in the context of ELT has a major downside as it requires a detector with a large number of pixels to satisfy at the same time the requirement on the extended spot sampling, both in term of pixel pitch and overall FOV, and on turbulence spatial sampling. [7][8][9] Although our work is general, it is particularly interesting for the tomographic AO systems of a couple of first light instruments of the ELT: multi-conjugate AO RelaY (MAORY) 10 and High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph (HARMONI). 11 We report in the following sections several examples derived from these instruments and the LGSWFS main parameters that we propose can be directly applied to them.…”

Section: Introductionmentioning

confidence: 99%

Key wavefront sensors features for laser-assisted tomographic adaptive optics systems on the Extremely Large Telescope

Fusco

Agapito

Neichel

et al. 2022

J. Astron. Telesc. Instrum. Syst.

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Laser guide star (LGS) wave-front sensing (LGSWFS) is a key element of tomographic adaptive optics system. However, when considering Extremely Large Telescope (ELT) scales, the LGS spot elongation becomes so large that it challenges the standard recipes to design LGSWFS. For classical Shack-Hartmann wave-front sensor (SHWFS), which is the current baseline for all ELT LGS-assisted instruments, a trade-off between the pupil spatial sampling [number of sub-apertures (SAs)], the SA field-of-view (FoV) and the pixel sampling within each SA is required. For ELT scales, this trade-off is also driven by strong technical constraints, especially concerning the available detectors and in particular their number of pixels. For SHWFS, a larger field of view per SA allows mitigating the LGS spot truncation, which represents a severe loss of performance due to measurement biases. For a given number of available detectors pixels, the SA FoV is competing with the proper sampling of the LGS spots, and/or the total number of SAs. We proposed a sensitivity analysis, and we explore how these parameters impacts the final performance. In particular, we introduce the concept of super resolution, which allows one to reduce the pupil sampling per WFS and opens an opportunity to propose potential LGSWFS designs providing the best performance for ELT scales.

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“…Despite being a forced choice for LGS sensing, the SHWFS in the context of ELT has a major downside as it requires a detector with a large number of pixels to satisfy at the same time the requirement on the extended spot sampling, both in term of pixel pitch and overall FoV, and on turbulence spatial sampling. [7][8][9] Although our work is general, it is particularly interesting for the tomographic adaptive optics systems of a couple of first light instruments of the ELT: MAORY 10 (Multi-conjugate Adaptive Optics RelaY) and HARMONI 11 (High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph). We report in the following sections several examples derived from these instruments and the LGSWFS main parameters that we propose can be directly applied to them.…”

Section: Introductionmentioning

confidence: 99%

Key wavefront sensors features for laser-assisted tomographic adaptive optics systems on the Extremely Large Telescope

Fusco,

Agapito,

Neichel

et al. 2022

Preprint

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Laser Guide Star [LGS] wave-front sensing [LGSWFS] is a key element of tomographic Adaptive Optics system. However, when considering Extremely Large Telescope [ELT] scales, the LGS spot elongation becomes so large that it challenges the standard recipes to design LGSWFS. For classical Shack-Hartmann Wave-Front Sensor [SHWFS], which is the current baseline for all ELT LGS-assisted instruments, a trade-off between the pupil spatial sampling (number of sub-apertures), the sub-aperture field-of-view and the pixel sampling within each sub-aperture is required. For ELT scales, this trade-off is also driven by strong technical constraints, especially concerning the available detectors and in particular their number of pixels. For SHWFS, a larger field of view per sub-aperture allows mitigating the LGS spot truncation, which represents a severe loss of performance due to measurement biases. For a given number of available detectors pixels, the sub-aperture Field of View [FoV] is competing with the proper sampling of the LGS spots, and/or the total number of sub-apertures. In this paper we propose a sensitivity analysis, and we explore how these parameters impacts the final performance. In particular we introduce the concept of super resolution, which allows to reduce the pupil sampling per WFS, and opens an opportunity to propose potential LGSWFS designs providing the best performance for ELT scales.

show abstract

MAORY: the adaptive optics module for the Extremely Large Telescope (ELT)

Cited by 13 publications

References 0 publications

TIPTOP: a new tool to efficiently predict your favorite AO PSF

TIPTOP: a new tool to efficiently predict your favorite AO PSF

Key wavefront sensors features for laser-assisted tomographic adaptive optics systems on the Extremely Large Telescope

Key wavefront sensors features for laser-assisted tomographic adaptive optics systems on the Extremely Large Telescope

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