High contrast imaging at the photon noise limit with WFS-based PSF calibration

Guyon, Olivier; Norris, Barnaby; Martinod, Marc-Antoine; Ahn, Kyohoon; Déo, Vincent; Skaf, Nour; Lozi, Julien; Vievard, Sébastien; Haffert, Sebastiaan Y.; Currie, Thayne; Males, Jared R.; Wong, Alison; Tuthill, P. G.

doi:10.1117/12.2630503

Cited by 3 publications

(4 citation statements)

References 17 publications

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“…Nevertheless, it is still limited by not only the existence of control rings, but also the objects of interest not superimposed on the control rings. We leave the handling of these limitations for future engineering (e.g., Guyon et al 2021) and methodological studies for potential joint works.…”

Section: Appendix A: Auxiliary Irdis Imaging Datamentioning

confidence: 99%

Protoplanetary disks in K_s-band total intensity and polarized light

Ren,

Benisty,

Ginski

et al. 2023

A&A

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Context. The diverse morphology among protoplanetary disks may result from planet-disk interactions, suggesting the presence of planets undergoing formation. The characterization of disks can provide information on the formation environments of planets. To date, most imaging campaigns have probed the polarized light from disks, which is only a fraction of the total scattered light and not very sensitive to planetary emission. Aims. We aim to observe and characterize protoplanetary disk systems in the near-infrared in both polarized and total intensity light to carry out an unprecedented study of the dust scattering properties of disks, as well as of any possible planetary companions. Methods. Using the star-hopping mode of the SPHERE instrument at the Very Large Telescope, we observed 29 young stars hosting protoplanetary disks and their reference stars in the Ks-band polarized light. We extracted disk signals in total intensity by removing stellar light using the corresponding reference star observations, by adopting the data imputation concept with sequential non-negative matrix factorization (DI-sNMF). For well-recovered disks in both polarized and total intensity light, we parameterized the polarization fraction phase functions using a scaled beta distribution. We investigated the empirical DI-sNMF detectability of disks using logistic regression. For systems with SPHERE data in the Y, J, and H bands, we have summarized their polarized color at an approximately 90° scattering angle. Results. We obtained high-quality disk images in total intensity for 15 systems and in polarized light for 23 systems. The total intensity detectability of disks primarily depends on the host star brightness, which determines adaptive-optics control ring imagery and thus stellar signals capture using DI-sNMF. The peak of polarization fraction tentatively correlates with the peak scattering angle, which could be reproduced using certain composition for compact dust, yet more detailed modeling studies are needed. Most of the disks are blue in polarized J – Ks color and the fact that they are relatively redder as stellar luminosity increases indicates larger scatterers. Conclusions. High-quality disk imagery in both total intensity and polarized light allows for disk characterizations in the polarization fraction. Combining these techniques reduces the confusion between the disk and planetary signals.

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Section: Appendix A: Auxiliary Irdis Imaging Datamentioning

confidence: 99%

Protoplanetary disks in K_s-band total intensity and polarized light

Ren,

Benisty,

Ginski

et al. 2023

A&A

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“…This interferometric approach to wavefront sensing is well-suited for a second-stage high-precision WFS/C following a more conventional AO correction so that starlight is efficiently coupled to the photonic device(s). These benefits have recently been demonstrated on-sky with the PL [87] and the GLINT instrument [88,89]. To fully realize this potential, the interferometric WFS output signals will need to be used for real-time active wavefront control, either by DM actuation or in-chip phase modulation.…”

Section: Symbiosis Between Adaptive Optics and Photonics: The Path To...mentioning

confidence: 99%

“…This architecture is particularly attractive for HCI, where a photonic nulling chip could iteratively reconfigure its internal phase delays [100] or drive external DM(s) to maintain optimal broadband null depths. By integrating science measurement and WFS functions within the same photonic chips, the stable relationship between WFS and science outputs can be measured and leveraged for self-calibration of science measurements down to the photon noise residual [88].…”

Section: Advances In Science and Technology To Meet Challengesmentioning

confidence: 99%

2023 Astrophotonics Roadmap: pathways to realizing multi-functional integrated astrophotonic instruments

Jovanovic,

Gatkine,

Anugu

et al. 2023

J. Phys. Photonics

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Photonic technologies offer numerous functionalities that can be used to realize astrophotonic instruments. The most spectacular example to date is the ESO Gravity instrument at the Very Large Telescope in Chile that combines the light-gathering power of four 8-m telescopes through a complex photonic interferometer. Fully integrated astrophotonic devices offer critical advantages for instrument development, including extreme miniaturization when operating at the diffraction-limit, plus integration, superior thermal and mechanical stabilization owing to the small footprint, and high replicability offering significant cost savings. Numerous astrophotonic technologies have been developed to address shortcomings of conventional instruments to date, including the development of photonic lanterns to convert from multimode inputs to single mode outputs, complex aperiodic fiber Bragg gratings to filter OH emission from the atmosphere, beam combiners enabling long baseline interferometry with for example, ESO Gravity, and laser frequency combs for high precision spectral calibration of spectrometers. Despite these successes, the facility implementation of photonic solutions in astronomical instrumentation is currently limited because of 1) low throughputs from coupling to fibers, coupling fibers to chips, propagation and bend losses, device losses, etc., 2) difficulties with scaling to large channel count devices needed for large bandwidths and high resolutions, and 3) efficient integration of photonics with detectors. In this roadmap, we identify 23 key areas that need further development. We outline the challenges and advances needed across those areas covering design tools, simulation capabilities, fabrication processes, the need for entirely new components, integration and hybridization and the characterization of devices. To realize these advances the astrophotonics community will have to work cooperatively with industrial partners who have more advanced manufacturing capabilities. With the advances described herein, multi-functional integrated instruments will be realized leading to novel observing capabilities for both ground and space based platforms, enabling new scientific studies and discoveries.

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“…in these proceedings. 22 The dramatic improvement in yield is illustrated by comparing Figure 12 to Figure 11.…”

Section: Exoplanet Yieldmentioning

confidence: 99%

The conceptual design of GMagAO-X: visible wavelength high contrast imaging with GMT

Males¹,

Close²,

Haffert³

et al. 2022

Preprint

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We present the conceptual design of GMagAO-X, an extreme adaptive optics system for the 25 m Giant Magellan Telescope (GMT). We are developing GMagAO-X to be available at or shortly after first-light of the GMT, to enable early high contrast exoplanet science in response to the Astro2020 recommendations. A key science goal is the characterization of nearby potentially habitable terrestrial worlds. GMagAO-Xis a woofer-tweeter system, with integrated segment phasing control. The tweeter is a 21,000 actuator segmented deformable mirror, composed of seven 3000 actuator segments. A multi-stage wavefront sensing system provides for bootstrapping, phasing, and high order sensing. The entire instrument is mounted in a rotator to provide gravity invariance. After the main AO system, visible (g to y) and near-IR (Y to H) science channels contain integrated coronagraphic wavefront control systems. The fully corrected and, optionally, coronagraphically filtered beams will then be fed to a suite of focal plane instrumentation including imagers and spectrographs. This will include existing facility instruments at GMT via fiber feeds. To assess the design we have developed an end-to-end frequencydomain modeling framework for assessing the performance of GMagAO-X. The dynamics of the many closed-loop feedback control systems are then modeled. Finally, we employ a frequency-domain model of post-processing algorithms to analyze the final post-processed sensitivity. The CoDR for GMagAO-X was held in September, 2021. Here we present an overview of the science cases, instrument design, expected performance, and concept of operations for GMagAO-X.

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High contrast imaging at the photon noise limit with WFS-based PSF calibration

Cited by 3 publications

References 17 publications

Protoplanetary disks in K_s-band total intensity and polarized light

Protoplanetary disks in K_s-band total intensity and polarized light

2023 Astrophotonics Roadmap: pathways to realizing multi-functional integrated astrophotonic instruments

The conceptual design of GMagAO-X: visible wavelength high contrast imaging with GMT

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High contrast imaging at the photon noise limit with WFS-based PSF calibration

Cited by 3 publications

References 17 publications

Protoplanetary disks in Ks-band total intensity and polarized light

Protoplanetary disks in Ks-band total intensity and polarized light

2023 Astrophotonics Roadmap: pathways to realizing multi-functional integrated astrophotonic instruments

The conceptual design of GMagAO-X: visible wavelength high contrast imaging with GMT

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Product

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Protoplanetary disks in K_s-band total intensity and polarized light

Protoplanetary disks in K_s-band total intensity and polarized light