GPI 2.0 : optimizing reconstructor performance in simulations and preliminary contrast estimates

Madurowicz, Alexander; Macintosh, Bruce; Poyneer, Lisa; Li, Duan; Ruffio, Jean-Baptiste; Véran, Jean-Pierre; Ammons, S. Mark; Savransky, Dmitry; Chilcote, Jeffrey; Maire, Jérôme; Konopacky, Quinn; Rosa, Robert J. De; Marois, Christian; Perrin, Marshall D.; Pueyo, Laurent

doi:10.1117/12.2563136

Cited by 4 publications

(3 citation statements)

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“…All the measurements are obtained with a 3λ∕D modulation, which is typical for such systems. 36 The software determines the correct masks to extract the four pupil images, from which 5640 X and Y slopes can be computed. A linear reconstructor is used to obtain an estimate of the 1603 modal coefficients from the slope vector for each wavefront map.…”

Section: Data Sourcementioning

confidence: 99%

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Mitigating the nonlinearities in a pyramid wavefront sensor

Archinuk,

Hafeez,

Fabbro

et al. 2023

J. Astron. Telesc. Instrum. Syst.

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For natural guide star adaptive optics (AO) systems, pyramid wavefront sensors (PWFSs) can provide a significant increase in sensitivity over the traditional Shack-Hartmann but at the cost of a reduced linear range. When using a linear reconstructor, nonlinearities result in wavefront estimation errors, which can have a significant impact on the image quality delivered by the AO system. We simulate a wavefront passing through a PWFS under varying observing conditions to explore the possibility of using a nonlinear machine learning model to estimate wavefront errors and compare with a linear reconstruction. We find significant potential improvements in delivered image quality even with computationally simple models, underscoring the need for further investigation of this approach.

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Section: Data Sourcementioning

confidence: 99%

“…Each PWFS image is captured on a 140×140 pixel grid. All the measurements are obtained with a 3λ/D modulation, which is typical for such systems 36 . The software determines the correct masks to extract the four pupil images, from which 5640 X and Y slopes can be computed.…”

Section: Data Sourcementioning

confidence: 99%

Mitigating the nonlinearities in a pyramid wavefront sensor

Archinuk,

Hafeez,

Fabbro

et al. 2023

J. Astron. Telesc. Instrum. Syst.

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“…The upgraded AO system will operate of 2kHz and will incorporate NUVU's HNü 240 which uses an E2V CCD 220. To estimate the Phyramid WFS's performance in GPI, the team has used PASSATA for AO simulations 39 and simulations of performance described in Madurowicz et al 40 Simulations of End-to-End AO performance is estimated to produce a Strehl ratio in H-band of at least 0.9 until 12th magnitude and to continue to operate, albeit with decreased performance, past 14th magnitude. While the Gemini North M2 print-through 41 and the GPI MEMS DM dead and coupled actuators 42 will affect final GPI contrast and science performance, they do not inhibit the simulated operations of the new GPI Pyramid WFS provided appropriately applied mitigation strategies.…”

Section: Ao Upgrade: Improving Contrast and Limiting Magnitudementioning

confidence: 99%

GPI 2.0: upgrading the Gemini Planet Imager

Chilcote

Konopacky

Rosa³

et al. 2020

Ground-Based and Airborne Instrumentation for Astronomy VIII

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The Gemini Planet Imager (GPI) is a dedicated high-contrast imaging facility designed for the direct detection and characterization of young Jupiter mass exoplanets. After six years of operation at Gemini South, GPI has helped establish that Jovian planets are rare at wide separations, but have higher occurrence rates at small separations. This motivates an upgrade of GPI to achieve deeper contrasts, especially at small inner working angles, while leveraging its current capabilities. GPI has been funded to undergo a major science-driven upgrade as part of a relocation to Gemini North (GN). Gemini plans to remove GPI at the end of 2020A. We present the status of the proposed upgrades to GPI including a EMCCD-based pyramid wavefront sensor, broadband low spectral resolution prisms and new apodized-pupil Lyot coronagraph designs. We discuss the expected

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Advances in control of a pyramid single conjugate adaptive optics system

Agapito

Rossi

Plantet

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Adaptive optics systems are an essential technology for the modern astronomy for ground based telescopes. One of the most recent revolution in the field is the introduction of the pyramid wavefront sensor. The higher performance of this device is payed with increased complexity in the control. In this work we report about advances in the AO system control obtained with SOUL at the Large Binocular Telescope. The first is an improved Tip/Tilt temporal control able to recover the nominal correction even in presence of high temporal frequency resonances. The second one is a modal gain optimization that has been successfully tested on sky for the first time. Pyramid wavefront sensors are the key technology for the first light AO systems of all ELTs and the reported advances can be relevant contributions for such systems.

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GPI 2.0 : optimizing reconstructor performance in simulations and preliminary contrast estimates

Cited by 4 publications

References 0 publications

Mitigating the nonlinearities in a pyramid wavefront sensor

Mitigating the nonlinearities in a pyramid wavefront sensor

GPI 2.0: upgrading the Gemini Planet Imager

Advances in control of a pyramid single conjugate adaptive optics system

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