The path to visible extreme adaptive optics with MagAO-2K and MagAO-X

Males, Jared R.; Close, Laird M.; Guyon, Olivier; Morzinski, Katie M.; Hinz, Philip M.; Esposito, Simone; Pinna, Enrico; Xompero, Marco; Briguglio, Runa; Riccardi, Armando; Puglisi, Alfio; Mazin, Ben; Ireland, Michael; Weinberger, Alycia J.; Conrad, Al; Kenworthy, Matthew A.; Snik, Frans; Otten, G. P. P. L.; Jovanović, Nemanja; Lozi, Julien

doi:10.1117/12.2234105

Cited by 14 publications

(14 citation statements)

References 54 publications

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“…Some initial studies have been done on wind measurement from GPI telemetry 24 and predictive Fourier control is being tested at ShaneAO, 25 but neither has been implemented on GPI. Several high contrast systems operate or have planned upgrades to operate at > 1 kHz, [26][27][28][29] to clear advantage with respect to lag errors. Additionally, GPI's WFS detector noise limits the system to guide stars of I < 10.…”

Section: Discussionmentioning

confidence: 99%

Status and performance of the Gemini Planet Imager adaptive optics system

et al. 2016

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The Gemini Planet Imager is a high-contrast near-infrared instrument specifically designed to image exoplanets and circumstellar disks over a narrow field of view. We use science data and AO telemetry taken during the first 1.5 yr of the GPI Exoplanet Survey to quantify the performance of the AO system. In a typical 60 sec H-band exposure, GPI achieves a 5σ raw contrast of 10 −4 at 0.4"; typical final 5σ contrasts for full 1 hr sequences are more than 10 times better than raw contrasts. We find that contrast is limited by bandwidth wavefront error over much of the PSF. Preliminary exploratory factor analysis can explain 60-70% of the variance in raw contrasts with combinations of seeing and wavefront error metrics. We also examine the effect of higher loop gains on contrast by comparing wavefront error maps reconstructed from AO telemetry to concurrent IFS images. These results point to several ways that GPI performance could be improved in software or hardware.

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Section: Discussionmentioning

confidence: 99%

Status and performance of the Gemini Planet Imager adaptive optics system

et al. 2016

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“…We applied our method to the cases of a 6.5 m circular aperture, here motivated by the indevelopment MagAO-X system. 47 We also consider a 25.4 m telescope, for which we used the collecting area of the GMT (seven 8.4 m segments), but ignored details of the aperture in PSD and contrast calculations. The parameters of our calculations for these telescopes are listed in Table 3.…”

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confidence: 99%

Ground-based adaptive optics coronagraphic performance under closed-loop predictive control

Males

Guyon

2018

J. Astron. Telesc. Instrum. Syst.

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The discovery of the exoplanet Proxima b highlights the potential for the coming generation of giant segmented mirror telescopes (GSMTs) to characterize terrestrial -potentially habitable -planets orbiting nearby stars with direct imaging. This will require continued development and implementation of optimized adaptive optics systems feeding coronagraphs on the GSMTs. Such development should proceed with an understanding of the fundamental limits imposed by atmospheric turbulence. Here we seek to address this question with a semi-analytic framework for calculating the post-coronagraph contrast in a closed-loop AO system. We do this starting with the temporal power spectra of the Fourier basis calculated assuming frozen flow turbulence, and then apply closed-loop transfer functions. We include the benefits of a simple predictive controller, which we show could provide over a factor of 1400 gain in raw PSF contrast at 1 λ/D on bright stars, and more than a factor of 30 gain on an I = 7.5 mag star such as Proxima. More sophisticated predictive control can be expected to improve this even further. Assuming a photon noise limited observing technique such as High Dispersion Coronagraphy, these gains in raw contrast will decrease integration times by the same large factors. Predictive control of atmospheric turbulence should therefore be seen as one of the key technologies which will enable ground-based telescopes to characterize terrrestrial planets.

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“…The development work invested in DARKNESS has simultaneously supported the MKID Exoplanet Camera (MEC), a 20 kilopixel MKID IFS for SCExAO shipping to Subaru in late 2017, and PICTURE-C (Cook et al 2015), a balloon-borne highcontrast platform that will fly a DARKNESS clone in 2019. Additionally, thanks to its portable design, DARKNESS is slated to join MagAO-X (Males et al 2016) in 2019 as the first high-contrast instrument with MKID IFS backend in the Southern Hemisphere.…”

Section: Conclusion and On-going Workmentioning

confidence: 99%

DARKNESS: A Microwave Kinetic Inductance Detector Integral Field Spectrograph for High-contrast Astronomy

Meeker

Mazin

Walter

et al. 2018

PASP

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We present DARKNESS (the DARK-speckle Near-infrared Energy-resolving Superconducting Spectrophotometer), the first of several planned integral field spectrographs to use optical/near-infrared Microwave Kinetic Inductance Detectors (MKIDs) for high-contrast imaging. The photon counting and simultaneous low-resolution spectroscopy provided by MKIDs will enable real-time speckle control techniques and post-processing speckle suppression at framerates capable of resolving the atmospheric speckles that currently limit high-contrast imaging from the ground. DARKNESS is now operational behind the PALM-3000 extreme adaptive optics system and the Stellar Double Coronagraph at Palomar Observatory. Here we describe the motivation, design, and characterization of the instrument, early on-sky results, and future prospects.

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The path to visible extreme adaptive optics with MagAO-2K and MagAO-X

Cited by 14 publications

References 54 publications

Status and performance of the Gemini Planet Imager adaptive optics system

Status and performance of the Gemini Planet Imager adaptive optics system

Ground-based adaptive optics coronagraphic performance under closed-loop predictive control

DARKNESS: A Microwave Kinetic Inductance Detector Integral Field Spectrograph for High-contrast Astronomy

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