The ESO Extremely Large Telescope instrumentation programme

Ramsay, S.; Amico, Paola; Bezawada, Naidu; Cirasuolo, M.; Dérie, F.; Egner, Sebastian; George, E. M.; Gonté, Frederic; Herrera, J. C. González; Hammersley, P. L.; Haupt, Christoph; Heijmans, Jeroen; Ives, Derek; Jakob, Gerd; Kerber, F.; Koehler, Bertrand; Mainieri, V.; Manescau, A.; Oberti, Sylvain; Padovani, P.; Péroux, Céline; Siebenmorgen, R.; Tamai, Roberto; Vernet, J.

doi:10.1117/12.2541400

Cited by 13 publications

(12 citation statements)

References 3 publications

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“…We can calculate this average DH contrast for any aberration vector directly, using the PASTIS matrix expression [Eq. (9)]. This is particularly interesting and efficient since it does not require E2E optical simulations and only involves simple linear algebra.…”

Section: Matrix Formalism To Calculate the Average Dark Hole Contrastmentioning

confidence: 99%

“…The Habitable Exoplanet Observatory 3 and the Large UV Optical Infrared Surveyor 4,5 (LUVOIR) are two space-based concepts recently studied by NASA as possible future flagship missions. Their primary science objective is the direct detection and spectral characterization of habitable Earth-like planets 6 and the search for life; they require primary mirror diameters of 4 to 15 m. Meanwhile, the ground-based community is preparing for the era of Extremely Large Telescopes (ELTs) where 30-to 40-m class telescopes such as the Thirty Meter Telescope 7 (TMT), the Giant Magellan Telescope 8 (GMT), and the European Extremely Large Telescope 9 (E-ELT) will be equipped with coronagraphs and extreme adaptive optics systems to search for and characterize exoplanets. 10 What unites all of these observatories is that they have significantly larger primary mirrors than their respective space-based and ground-based predecessors.…”

Section: Introductionmentioning

confidence: 99%

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Analytical tolerancing of segmented telescope co-phasing for exo-Earth high-contrast imaging

Laginja

Soummer

Mugnier

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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This paper introduces an analytical method to calculate segment-level wavefront error (WFE) tolerances to enable the detection of faint extra-solar planets using segmentedaperture telescopes in space. This study provides a full treatment of the case of spatially uncorrelated segment phasing errors for segmented telescope coronagraphy, which has so far only been approached using ad-hoc Monte Carlo (MC) simulations. Instead of describing the wavefront tolerance globally for all segments, our method produces spatially dependent requirement maps. We relate the statistical mean contrast in the coronagraph dark hole to the standard deviation of the WFE of each individual segment on the primary mirror. This statistical framework for segment-level tolerancing extends the Pair-based Analytical model for Segmented Telescope Imaging from Space (PASTIS), which is based uniquely on a matrix multiplication for the optical propagation. We confirm our analytical results with MC simulations of end-to-end optical propagations through a coronagraph. Comparing our results for the Apodized Pupil Lyot Coronagraph designs for the Large Ultraviolet Optical Infrared telescope to previous studies, we show general agreement but we provide a relaxation of the requirements for a significant subset of segments in the pupil. These requirement maps are unique to any given telescope geometry and coronagraph design. The spatially uncorrelated segment tolerances we calculate are a key element of a complete error budget that will also need to include allocations for correlated segment contributions. We discuss how the PASTIS formalism can be extended to the spatially correlated case by deriving the statistical mean contrast and its variance for a nondiagonal aberration covariance matrix. The PASTIS tolerancing framework therefore brings a new capability that is necessary for the global tolerancing of future segmented space observatories.

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Section: Matrix Formalism To Calculate the Average Dark Hole Contrastmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Analytical tolerancing of segmented telescope co-phasing for exo-Earth high-contrast imaging

Laginja

Soummer

Mugnier

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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“…An overall gradient between higher fractions in the southwest and lower fractions in the northeast is consistent with the decrease of MCB‐landfall frequency from south to north (Figure S1 in Supporting Information ) and the increase of summertime convection toward the Altiplano in the northeast (Garreaud, 1999). Maximum fractional precipitation appears in an area between 23°S and 24°S bounded by the city of Antofagasta in the west, stretching into the central valley to the east and just slightly north of the European Southern Observatory's construction site for the world's largest optical telescope (Cantalloube et al., 2020; Ramsay et al., 2020). For this region, more than 70% of the total precipitation is associated with MCBs making landfall.…”

Section: Composite Analysismentioning

confidence: 99%

The Role of Moisture Conveyor Belts for Precipitation in the Atacama Desert

Böhm

Reyers

Knarr

et al. 2021

Geophysical Research Letters

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“…The ground-based GSMTs include the Thirty Meter Telescope (TMT), 5 the Giant Magellan Telescope (GMT), 6 and the European Extremely Large Telescope (E-ELT). 7 Various testbeds are advancing technology and techniques to enable exoplanet imaging on the next generation of telescopes.…”

Section: Introductionmentioning

confidence: 99%

Three-sided pyramid wavefront sensor, part II: preliminary demonstration on the new comprehensive adaptive optics and coronagraph test instrument testbed

Schatz

Codona

Long

et al. 2022

J. Astron. Telesc. Instrum. Syst.

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The next generation of giant ground and space telescopes will have the light-collecting power to detect and characterize potentially habitable terrestrial exoplanets using high-contrast imaging for the first time. This will only be achievable if the performance of Giant Segmented Mirror Telescopes (GSMTs) extreme adaptive optics (ExAO) systems are optimized to their full potential. A key component of an ExAO system is the wavefront sensor (WFS), which measures aberrations from atmospheric turbulence. A common choice in current and next-generation instruments is the pyramid wavefront sensor (PWFS). ExAO systems require high spatial and temporal sampling of wavefronts to optimize performance, and as a result, require large detectors for the WFS. We present a closed-loop testbed demonstration of a three-sided pyramid wavefront sensor (3PWFS) as an alternative to the conventional four-sided pyramid wavefront (4PWFS) sensor for GSMT-ExAO applications on the new Comprehensive Adaptive Optics and Coronagraph Test Instrument (CACTI). The 3PWFS is less sensitive to read noise than the 4PWFS because it uses fewer detector pixels. The 3PWFS has further benefits: a high-quality three-sided pyramid optic is easier to manufacture than a four-sided pyramid. We detail the design of the two components of the CACTI system, the adaptive optics simulator and the PWFS testbed that includes both a 3PWFS and 4PWFS. We detail the error budget of the CACTI system, review its operation and calibration procedures, and discuss its current status. A preliminary experiment was performed on CACTI to study the performance of the 3PWFS to the 4PWFS in varying strengths of turbulence using both the Raw Intensity and Slopes Map signal processing methods. This experiment was repeated for a modulation radius of 1.6 λ/D and 3.25 λ/D. We found that the performance of the two wavefront sensors is comparable if modal loop gains are tuned.

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The ESO Extremely Large Telescope instrumentation programme

Cited by 13 publications

References 3 publications

Analytical tolerancing of segmented telescope co-phasing for exo-Earth high-contrast imaging

Analytical tolerancing of segmented telescope co-phasing for exo-Earth high-contrast imaging

The Role of Moisture Conveyor Belts for Precipitation in the Atacama Desert

Three-sided pyramid wavefront sensor, part II: preliminary demonstration on the new comprehensive adaptive optics and coronagraph test instrument testbed

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