Author: "Jean-François Sauvage" - Searchworks@Jio Institute Digital Library Search Results

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148 results on '"Jean-François Sauvage"'

1. Active deployable primary mirrors on CubeSat

Author: Schwartz, Noah, Milanova, Maria, Brzozowski, William, Todd, Stephen, Ali, Zeshan, Buron, Lucie, Jean-François-Sauvage, Bond, Charlotte, Bruce, Heather, Rees, Phil, Ferrari, Marc, and MacLeod, Donald
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Space Physics
Abstract: The volume available on small satellites restricts the size of optical apertures to a few centimetres, limiting the Ground-Sampling Distance (GSD) in the visible to typically 3 m at 500 km. We present in this paper the latest development of a laboratory demonstrator of a segmented deployable telescope that will triple the achievable ground resolution and improve photometric capability of CubeSat imagers. Each mirror segment is folded for launch and unfolds in space. We demonstrate through laboratory validation very high deployment repeatability of the mirrors <{\pm}5 {\mu}m. To enable diffraction-limited imaging, segments are controlled in piston, tip, and tilt. This is achieved by an initial coarse alignment of the mirrors followed by a fine phasing step. Finally, we investigate the impact of the thermal environment on high-order wavefront error and the conceptual design of a deployable secondary fitting inside 1U., Comment: Proceedings of 13th IAA Symposium on Small Satellites for Earth Observation (SSSEO 2021)
Published: 2021

2. Feasibility demonstration of AO pre-compensation for GEO feeder links in a relevant environment

Author: Aurélie Montmerle, Bonnefois, Marie-Thérése, Velluet, Mahawa, Cissé, Caroline B, Lim, Jean-Marc, Conan, Cyril, Petit, Jean-François, Sauvage, Serge, Meimon, Philippe, Perrault, Joseph, Montri, and Nicolas, Védrenne
Abstract: Optical technologies are extremely competitive candidates to achieve very-high throughput links between ground and GEO satellites; however, their feasibility relies on the ability to mitigate channel impairments due to atmospheric turbulence. For that purpose, Adaptive Optics (AO) has already proved to be highly efficient on the downlink. However, for the uplink, anisoplanatism induced by point-ahead angle (PAA) compromises AO pre-compensation efficiency to an extent that depends on propagation conditions. The ability to properly assess the anisoplanatism impact in a wide variety of conditions is thus critical in designing the optical ground terminals. In this paper, we demonstrate the consistency of experimental coupled flux statistics with results coming from performance and end-to-end models, on an AO pre-compensated 13 km slant path in Tenerife. This validation is demonstrated in a wide variety of turbulence conditions, hence consolidating propagation channel models that are of critical importance for the reliability of future GEO feeder links. We then compare experimental results to theoretical on-sky performance, and discuss to what extent such slant path or horizontal path experiments can be representative of real GEO links.
Published: 2022

3. PSF nowcast using PASSATA simulations -- Towards a PSF forecast

Author: Alessio Turchi, Guido Agapito, Elena Masciadri, Olivier A. Beltramo-Martin, Julien Milli, Cédric Plantet, Fabio Rossi, Enrico Pinna, Jean-François Sauvage, Benoît Neichel, Thierry Fusco, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: Characterizing the PSF of adaptive optics instruments is of paramount importance both for instrument design and observation planning/optimization. Simulation software, such as PASSATA, have been successfully utilized for PSF characterization in instrument design, which make use of standardized atmospheric turbulence profiles to produce PSFs that represent the typical instrument performance. In this contribution we study the feasibility of using such tool for nowcast application (present-time forecast), such as the characterization of an on-sky measured PSF in real observations. Specifically we will analyze the performance of the simulation software in characterizing the real-time PSF of two different state-of-the-art SCAO adaptive optics instruments: SOUL at the LBT, and SAXO at the VLT. The study will make use of on-sky measurements of the atmospheric turbulence and compare the results of the simulations to the measured PSF figures of merit (namely the FHWM and the Strehl Ratio) retrieved from the instrument telemetry in real observations. Our main goal in this phase is to quantify the level of uncertainly of the AO simulations in reproducing real on-sky observed PSFs with an end-to-end code (PASSATA). In a successive phase we intend to use a faster analytical code (TIPTOP). This work is part of a wider study which aims to use simulation tools joint to atmospheric turbulence forecasts performed nightly to forecast in advance the PSF and support science operations of ground-based telescopes facilities. The 'PSF forecast' option might therefore be added to ALTA Center or the operational forecast system that will be implemented soon at ESO., 10 pages, 6 figures
Published: 2022

4. Adapter le senseur pyramide pour la fragmentation pupillaire des télescopes de classe ELT

Author: Nicolas Levraud, Vincent Chambouleyron, Olivier Fauvarque, Mahawa Cissé, Jean-François Sauvage, Benoît Neichel, Charlotte Z. Bond, Enrico Pinna, Simone Esposito, Noah Schwartz, Thierry Fusco, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), DOTA, ONERA [Salon], ONERA, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), DOTA, ONERA, Université Paris Saclay [Palaiseau], ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018), Laboratoire Détection Capteurs et Mesure (LDCM), Recherches et Développements Technologiques (RDT), and Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)
Subjects: ELT, [PHYS]Physics [physics], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Segmented Telescope, Pyramid Wavefront Sensor, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SPI]Engineering Sciences [physics], Optique adaptative, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Adaptive optics -instrumentation, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Analyse Surface d'Onde
Abstract: International audience; The next generation of Extremely Large Telescope (24 to 39m diameter) will suffer from the so-called "pupil fragmentation" problem. Due to their pupil shape complexity (segmentation, large spiders ...), some differential pistons may appear between some isolated part of the full pupil during the observations. Although classical AO system will be able to correct for turbulence effects, they will be blind to this specific telescope induced perturbations. Hence, such differential piston, a.k.a petal modes, will prevent to reach the diffraction limit of the telescope and ultimately will represent the main limitation of AO-assisted observation with an ELT. In this work we analyse the spatial structure of these petal modes and how it affects the ability of a Pyramid Wavefront sensor to sense them. Then we propose a variation around the classical Pyramid concept for increasing the WFS sensitivity to this particular modes. Nevertheless, We show that one single WFS can not accurately and simultaneously measure turbulence and petal modes. We propose a double path wavefront sensor scheme to solve this problem. We show that such a scheme,associated to a spatial filtering of residual turbulence in the second WFS path dedicated to petal mode sensing, allows to fully measure and correct for both turbulence and fragmentation effects and will eventually restore the full capability and spatial resolution of the future ELT.; La prochaine génération de Télescope Extrêmement Large (de 24 a 39m de diamètre) souffrira du problème de fragmentation de la pupille. Du a la complexité de la pupille de ces télescopes (segmentation, grande araignée, ...) des différences de piston peuvent apparaître entre les fragments de la pupille. Les systèmes d'Optique adaptative (OA) censées corrigés l'effet de turbulence seront aveugles a ces perturbations induites par la structure du télescope. Ces effets de piston différentiels souvent nommés mode pétale nous empêcheront d'atteindre la limite de diffraction du télescope et peut représenter la limite des observations assistés par Optique Adaptatives. Dans ce travail nous étudions la structure spatial de ces modes pétales et comment cela affecte la capacité du senseur pyramide a le mesurer. Ensuite nous proposons une modification du senseur pyramide pour améliorer la sensibilité au mode pétale. Néanmoins, nous avons montré qu'un seul ne peut pas être efficace pour mesurer en même temps la turbulence et les modes pétales. Nous proposons un senseur a deux voies pour résoudre ce problème. Nous montrons aussi qu'un tel schéma, associé a un filtrage spatial des résidus de turbulence permet de mesurer plus complétement et corriger la turbulence et les effets de fragmentation et finalement permet de restaurer la capacité et résolution compléte des futurs ELT.
Published: 2022

5. HARMONI at ELT: system analysis and performance estimation of the high-contrast module

Author: Alexis Carlotti, Laurent Jocou, Thibaut Moulin, Patrick Rabou, Alexis Bidot, Adrien Hours, Yves Magnard, Alain Delboulbé, Fabrice Pancher, Élodie Choquet, Arthur Vigan, Mathis Houllé, Kjetil Dohlen, Jean-François Sauvage, Thierry Fusco, Niranjan Thatte, Benoît Neichel, Fraser Clarke, Dave Melotte, Matthias Tecza, Hermine Schnetler, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA [Salon], ONERA, DOTA, ONERA, Université Paris Saclay [Palaiseau], and ONERA-Université Paris-Saclay
Subjects: ELT, high spectral resolution, [PHYS]Physics [physics], [SPI]Engineering Sciences [physics], exoplanets, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], direct imaging, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Spectroscopy, high angular resolution, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 450nm to 2450nm with resolving powers from 3500 to 18000 and spatial sampling from 60mas to 4mas. It can operate in two Adaptive Optics modes- SCAO (including a High Contrast capability) and LTAOor with NOAO. The project is preparing for Final Design Reviews. The high-contrast module (HCM) has been designed to characterize planets as close as 100mas from their host star (goal: 50mas), and presenting a 1e-6 f lux ratio with it. To do so, it will use (1) a passive atmospheric dispersion corrector, (2) a set of amplitude apodizers and focal plane masks to lower the di↵racted intensity next to the star and attenuate the PSF core, (3) a dedicated Zernike wavefront sensor to track the non-common path aberrations with the SCAO subsystem at a 0.1Hz frequency, and (4) post-processing algorithms that will rely on the temporal and spectral diversity of the IFS data to separate the planetary signals from the noise. This communication details several trade-o↵ analyses involved in the co-design of the hardware of the HCM. It also presents contrast performance estimates that have been derived through an analysis of post-processed, simulated IFS data obtained with an end-to-end numerical model of the HCM and the rest of HARMONI. The respective interests of ADI and molecular mapping are compared in this specific case.
Published: 2022

6. HARMONI sur l'ELT : un analyseur de front d'onde de Zernike pour le module Haut-Contraste : résultats expérimentaux dans des conditions réalistes d'observation

Author: Adrien Hours, Alexis Carlotti, David Mouillet, Alain Delboulbé, Sylvain Guieu, Laurent Jocou, Thibaut Moulin, Fabrice Pancher, Patrick Rabou, Élodie Choquet, Kjetil Dohlen, Jean François Sauvage, Mamadou N'Diaye, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA [Salon], ONERA, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: ELT, [SDU]Sciences of the Universe [physics], FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, OPTIQUE ADAPTATIVE, Instrumentation and Methods for Astrophysics (astro-ph.IM), EXOPLANETE
Abstract: ELT-HARMONI is the first light visible and near-IR integral field spectrograph (IFS) for the ELT. It covers a large spectral range from 450nm to 2450nm with resolving powers from 3500 to 18000 and spatial sampling from 60mas to 4mas. It can operate in two Adaptive Optics modes - SCAO (including a High Contrast capability) and LTAO - or with NOAO. The project is preparing for Final Design Reviews. The High Contrast Module (HCM) will allow HARMONI to perform direct imaging and spectral analysis of exoplanets up to one million times fainter than their host star. Quasi-static aberrations are a limiting factor and must be calibrated as close as possible to the focal plane masks to reach the specified contrast. A Zernike sensor for Extremely Low-level Differential Aberrations (ZELDA) will be used in real-time and closed-loop operation at 0.1Hz frequency for this purpose. Unlike a Shack-Hartmann, the ZELDA wavefront sensor is sensitive to Island and low-wind effects. The ZELDA sensor has already been tested on VLT-SPHERE and will be used in other instruments. Our objective is to adapt this sensor to the specific case of HARMONI. A ZELDA prototype is being both simulated and experimentally tested at IPAG. Its nanometric precision has first been checked in 2020 in the case of slowly evolving, small wavefront errors, and without dispersion nor turbulence residuals. On this experimental basis, we address the performance of the sensor under realistic operational conditions including residuals, mis-centring, dispersion, sensitivity, etc. Atmospheric refraction residuals were introduced by the use of a prism, and turbulence was introduced by a spatial light modulator which is also used to minimise wavefront residuals in a closed loop in the observing conditions expected with HARMONI., 14 pages, 13 figures, SPIE Astronomical Telescopes + Instrumentation (AS22)
Published: 2022

7. Laboratory demonstration of focal plane wavefront sensing using phase diversity: a way to tackle the problem of NCPA in SHARK-NIR. Part II: new characterization tests and alternative wavefront sensing strategies

Author: Daniele Vassallo, Maria Bergomi, Elena Carolo, Davide Greggio, Luca Marafatto, Gabriele Umbriaco, Jacopo Farinato, Andrea Baruffolo, Kalyan Kumar Radhakrishnan Santhakumari, Valentina Viotto, Jean-François Sauvage, and Thierry Fusco
Published: 2022

8. Experimental validation of exoplanet centring strategies for high dispersion coronagraphy

Author: Mona El Morsy, Arthur Vigan, Maxime Lopez, Gilles P. P. L. Otten, Élodie Choquet, Fabrice Madec, Anne Costille, Jean-François Sauvage, Kjetil Dohlen, Eduard R. Muslimov, Raphaël Pourcelot, Johan Floriot, Jean-Antoine Benedetti, Patrick Blanchard, Philippe Balard, Graham J. Murray, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), and University of Cambridge [UK] (CAM)
Subjects: fibre optique monomode, [PHYS]Physics [physics], [SPI]Engineering Sciences [physics], optique adaptative
Abstract: International audience; The combination on large ground-based telescopes of extreme adaptive optics (ExAO), coronagraphy and high-dispersion spectroscopy is starting to emerge as a powerful technique for the direct characterisation of giant exoplanets. High spectral resolution not only brings a major gain in terms of accessible spectral features, but it also enables to better disentangle between the stellar and planetary signals thanks to the much higher spectral content. On-going projects such as KPIC for Keck, REACH for Subaru and HiRISE for the VLT base their observing strategy on the use of a few science fibres, one of which is dedicated to sampling the PSF of the planet, while the others sample the stellar residuals in the speckle field. The main challenge in this approach is to blindly centre the science fibre on the planet’s PSF, with typically a tolerance of less than one resolution element (0.1 λ/D). Several possible centring strategies can be adopted, either based on calibration fibres retro-injecting signal to mark the position of the science fibres or based on the use of focal-plane features introduced by the ExAO system. In this proceeding, we describe different possible approaches and we compare their centring accuracy using the MITHiC high-contrast imaging testbed. For this work, MITHiC has been upgraded to reproduce a setup close to the one that will be adopted in HiRISE, the coupling system that will soon be implemented between VLT/SPHERE and VLT/CRIRES+. Our results demonstrate that reaching a specification accuracy of 0.1 λ/D is extremely challenging regardless of the chosen centring strategy. It requires a high level of accuracy at every step of the centring procedure, which can be reached with very stable instruments. We studied the contributors to the centring error in the case of MITHiC and we quantified some of the most important terms.
Published: 2022

9. First light for PAPYRUS, the pyramid based adaptive optics system at LAM/OHP

Author: Vincent Chambouleyron, Idir Boudjema, Romain Fétick, Eduard R. Muslimov, Felipe Pedreros Bustos, Nicolas Levraud, Esther Soria Hernandez, Amandine Caillat, Jérôme Schmitt, Jean-François Sauvage, Benoît Neichel, Thierry Fusco, Mahawa Cissé, Maxime Massa, François Leroux, Fabrice Madec, Sonia Karkar, Kacem El-Hadi, Alexis Lau, and Romain Lhoussaine
Published: 2022

10. Opto-mechanical model of AZIMOV, the deployable telescope for CubeSat

Author: Jean-François Sauvage, Noah Schwartz, Lucie Buron, Zeshan Ali, Maxime Dumont, Marc Ferrari, Johan Petit, Pascal Vola, Marc Jaquet, Tony Pamplona, Bernard Rosier, Antoine Miniussi, and Vincent Michau
Published: 2022

11. 6U CubeSat deployable telescope for optical Earth observation and astronomical optical imaging

Author: Noah Schwartz, William Brzozowski, Zeshan Ali, Maria Milanova, Katherine Morris, Charlotte Bond, Jennifer Keogh, Douglas Harvey, Lawrence Bissell, Jean-François Sauvage, Maxime Dumont, Carlos Correia, Phil Rees, and Heather Bruce
Published: 2022

12. Deep learning for space-borne focal-plane wavefront sensing

Author: Maxime Dumont, Carlos Correia, Jean-François Sauvage, Noah Schwartz, Morgan Gray, Olivier Beltramo-Martin, Jaime Cardoso, CRETIN, Dorine, DOTA, ONERA [Salon], ONERA, Space ODT - Optical Deblurring Technologies, UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), SpaceAble, Faculdade de Engenharia da Universidade do Porto (FEUP), and Universidade do Porto = University of Porto
Subjects: [PHYS]Physics [physics], APPRENTISSAGE AUTOMATIQUE, [SPI] Engineering Sciences [physics], Astronomy, CubeSat, Neural Network, Deep learning, Nanosatellite, [PHYS] Physics [physics], [SPI]Engineering Sciences [physics], Artificial Intelligence, ANALYSE SURFACE ONDE, Focal plane wavefront sensing, Wavefront sensing
Abstract: For space-based Earth Observations and solar system observations, obtaining both high revisit rates (using a constellation of small platforms) and high angular resolution (using large optics and therefore a large platform) is an asset for many applications. Unfortunately, they prevent the occurrence of each other. A deployable satellite concept has been suggested that could grant both assets by producing jointly high revisit rates and high angular resolution of roughly 1 meter on the ground. This concept relies however on the capacity to maintain the phasing of the segments at a sufficient precision (a few tens of nanometers at visible wavelengths), while undergoing strong and dynamic thermal gradients. In the constrained volume environment of a CubeSat, the system must reuse the scientific images to measure the phasing errors. We address in this paper the key issue of focal-plane wave-front sensing for a segmented pupil using a single image with deep learning. We show a first demonstration of measurement on a point source. The neural network is able to identify properly the phase piston-tip-tilt coefficients below the limit of 15nm per petal., Pour les observations spatiales de la Terre et du système solaire, l'obtention à la fois de taux de revisite élevés (en utilisant une constellation de petites plates-formes) et une haute résolution angulaire (en utilisant de grandes optiques et donc une grande plate-forme) est un atout pour de nombreuses applications. Malheureusement, elles s'excluent l'une et de l'autre. Un concept de satellite déployable a été suggéré, qui pourrait garantir ces deux atouts en produisant conjointement des taux de revisite élevés et une haute résolution angulaire d'environ 1 mètre au sol.Ce concept repose cependant sur la capacité à maintenir le phasage des segments à une précision suffisante (quelques dizaines de nanomètres aux longueurs d'onde visibles), tout en subissant des gradients thermiques forts et dynamiques. Dans l'environnement volumique contraint d'un CubeSat, le système doit réutiliser les images scientifiques pour mesurer leserreurs de phasage.Nous abordons dans cet article le problème clé de la détection du front d'onde du plan focal pour une pupille segmentée en utilisant une seule image avec l'apprentissage profond. Nous montrons une première démonstration de mesure sur une source ponctuelle.Le réseau neuronal est capable d'identifier correctement les coefficients de phase piston-pointe-inclinaison en dessous de la limite de 15nm par pétale.
Published: 2022

13. HARMONI at ELT: adaptive optics calibration unit from design to prototyping

Author: Noah Schwartz, Edgard Renault, William Ceria, Martin Black, Kjetil Dohlen, Kacem El Hadi, Jean François Sauvage, Lisa F. Bardou, Timothy J. Morris, Benoit Neichel, Thierry Fusco, Fraser Clarke, Dave Melotte, Niranjan Thatte, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA [Salon], ONERA, DOTA, ONERA, Université Paris Saclay [Palaiseau], and ONERA-Université Paris-Saclay
Subjects: ELT, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], calibration source, aberrations, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Adaptive optics, natural guide star, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; In this paper, we present the design and prototyping of the HARMONI Adaptive Optics Calibration Unit (AOCU). The AOCU consists of a set of on-axis sources (covering 0.5-2.4 µm) with a controllable wavefront shape. It will deploy into the instrument focal plane to inject calibration light into the rest of the system. The AOCU supports all-natural guide-star wavefront sensors for SCAO, HCAO, and LTAO. The AOCU will be used to calibrate the WFSs, the internal interaction matrices of HARMONI, measure and compensate NCPAs between AO dichroics and the science detectors, and calibrate the pointing model zero position. The illumination assembly of the AOCU will consist of six diffraction-limited sources and a resolved source coupled into fibres. Because of the wide range of wavelengths and the spatial separations requirements, we use two endlessly single-mode fibres and a multimode fibre. In addition, several LED sources need to be coupled efficiently into the single-mode fibres. In this paper, we present the general AOCU design using off-the-shelf with a focus on the illumination and source module.
Published: 2022

14. HARMONI at ELT: prototyping for Single-Conjugate AO Sensor subsystem

Author: Kacem El Hadi, Jean-François Sauvage, Kjetil Dohlen, Edgard Renault, William Bon, Pascal Vola, Thibaut Crauchet, Louis Gemmerle, Fabrice Madec, David Le Mignant, Benoit Neichel, Thierry Fusco, Fraser Clarke, Dave J. Melotte, Matthias Tecza, Niranjan Thatte, Jérôme Amiaux, Jérôme Paufique, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA [Salon], ONERA, DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018), ANR-19-CE31-0011,APPLY,Prédiction de la réponse impulsionnelle pour les obervations assitées par Optique Adaptative(2019), and ANR-21-ESRE-0008,F-CELT,Contribution Française à l'instrumentation de l'Extremely Large Telescope(2021)
Subjects: Pyramid, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Tip-Tilt Mechanism, Adaptive Optics, modulator, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Wave-Front Sensing, ELT HARMONI, SCAO, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 450nm to 2450nm with resolving powers from 3500 to 18000 and spatial sampling from 60mas to 4mas. It can operate in two Adaptive Optics modes-SCAO (including a High Contrast capability) and LTAO-or with NOAO. The project is preparing for Final Design Reviews. The SCAO Sensors subsystem (SCAOS) is located within the Natural Guide Star Sensors (NGSS) system which includes several wavefront sensors (WFS) to cover the needs of the different HARMONI observing modes and operates in a cold, thermally stabilized (+2°C) and dry gas environment for thermal background limitation. To reach the required performance, the SCAOS will use different modules and mechanisms among which, two particularly critical devices have been prototyped and are tested: The SCAOS Pyramid Modulator Unit (SPMU) and the SCAOS Object Selection Mechanism (SOSM). Both devices are tip-tilt mirrors but have very different specifications (amplitude and speed). In this work, we will present and discuss the design, the assembly and the full test (performance, control) of the two systems, in both ambient and cold environments.
Published: 2022

15. HARMONI sur l'ELT : contrôle de front d'onde pour le mode SCAO

Author: Charlotte Z. Bond, Jean-François Sauvage, Noah Schwartz, Nicolas Levraud, Vincent Chambouleyron, Carlos M. Correia, Thierry Fusco, Benoit Neichel, DOTA, ONERA [Salon], ONERA, DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018), ANR-19-CE31-0011,APPLY,Prédiction de la réponse impulsionnelle pour les obervations assitées par Optique Adaptative(2019), and ANR-21-ESRE-0008,F-CELT,Contribution Française à l'instrumentation de l'Extremely Large Telescope(2021)
Subjects: ELT, [PHYS]Physics [physics], [SPI]Engineering Sciences [physics], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], OPTIQUE ADAPTATIVE, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 450nm to 2450nm with resolving powers from 3500 to 18000 and spatial sampling from 60mas to 4mas. It can operate in two Adaptive Optics (AO) modes - SCAO (including a High Contrast capability) and LTAO - or with NOAO. The project is preparing for Final Design Reviews.The SCAO system for HARMONI is based on a pyramid wavefront sensor (PWFS) operating in the visible (700 – 1000 nm). Previous implementations on very large telescopes have demonstrated the challenges associated with optimising PWFS performance on-sky, particularly when operated at visible wavelengths. ELT operation will pose further challenges for AO systems, particularly related to the segmentation of the telescope and the control of badly seen ‘petal modes’. In this paper we investigate these challenges in the context of the HARMONI SCAO system. We present the results of end-to-end simulations of our baseline approach, using a coupled control basis to avoid the runaway development of petal modes in the control loop. The impact of key parameters are investigated and methods for optical gain compensation and optimisation of the control basis are presented. We discuss recent updates to the control algorithms and demonstrate the possibility of improving performance using a form of super resolution. Finally, we report on the expected performance across a range of conditions.
Published: 2022

16. Imageur à haut contraste pour les télescopes à ouverture complexe (HICAT) : 8. Démonstration de Dark Zone avec boucles fermées simultanées à bas ordres

Author: Rémi Soummer, Emiel H. Por, Raphaël Pourcelot, Susan F. Redmond, Iva Laginja, Scott D. Will, Marshall D. Perrin, Laurent Pueyo, Ananya Sahoo, Peter Petrone, Keira J. Brooks, Rachel Fox, Alex Klein, Bryony Nickson, Thomas Comeau, Marc Ferrari, Rob Gontrum, John Hagopian, Lucie Leboulleux, Daniel Leongomez, Joe Lugten, Laurent M. Mugnier, Mamadou N'Diaye, Meiji Nguyen, James Noss, Jean-François Sauvage, Nathan Scott, Anand Sivaramakrishnan, Hari B. Subedi, Sam Weinstock, Space Telescope Science Institute (STSci), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Department of Mechanical and Aerospace Engineering [Princeton] (MAE), Princeton University, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, Université Paris sciences et lettres (PSL), NASA Goddard Space Flight Center (GSFC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Advanced Nanophotonics, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, DOTA, ONERA [Salon], ONERA, Johns Hopkins University (JHU), and NASA
Subjects: GOMaP, [PHYS]Physics [physics], [SPI]Engineering Sciences [physics], LUVEx, OPTIQUE ACTIVE, Coronagraphy high-contrast GOMaP LUVEx LUVOIR, high-contrast, LUVOIR, Coronagraphy, EXOPLANETE
Abstract: International audience; We present recent laboratory results demonstrating high-contrast coronagraphy for the future space-based large IR/Optical/Ultraviolet telescope recommended by the Decadal Survey. The High-contrast Imager for Complex Aperture Telescopes (HiCAT) testbed aims to implement a system-level hardware demonstration for segmented aperture coronagraphs with wavefront control. The telescope hardware simulator employs a segmented deformable mirror with 37 hexagonal segments that can be controlled in piston, tip, and tilt. In addition, two continuous deformable mirrors are used for high-order wavefront sensing and control. The low-order sensing subsystem includes a dedicated tip-tilt stage, a coronagraphic target acquisition camera, and a Zernike wavefront sensor that is used to measure and correct low-order aberration drifts. We explore the performance of a segmented aperture coronagraph both in "static" operations (limited by natural drifts and instabilities) and in "dynamic" operations (in the presence of artificial wavefront drifts added to the deformable mirrors), and discuss the estimation and control strategies used to reach and maintain the dark-zone contrast using our low-order wavefront sensing and control. We summarize experimental results that quantify the performance of the testbed in terms of contrast, inner/outer working angle and bandpass, and analyze limiting factors.
Published: 2022

17. Wavefront tolerances of space-based segmented telescopes at very high contrast: Experimental validation

Author: Scott D. Will, Laurent Pueyo, Iva Laginja, Laurent M. Mugnier, James Noss, Peter Petrone, Rémi Soummer, Emiel H. Por, Jean-François Sauvage, Keira Brooks, Marshall D. Perrin, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Space Telescope Science Institute (STSci), University of Rochester [USA], Hexagon Federal, This work was supported by the Action Spécifique Haute Résolution Angulaire (ASHRA) of CNRS/INSU co-funded by CNES. This work was also supported in part by the National Aeronautics and Space Administration under Grant 80NSSC19K0120 issued through the Strategic Astrophysics Technology/Technology Demonstration for Exoplanet Missions Program (SAT-TDEM, PI: R. Soummer). E. H. P is supported by the NASA Hubble Fellowship grant #HST-HF2-51467.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555., and ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018)
Subjects: planets and satellites: detection, Segmented mirror, Aperture, FOS: Physical sciences, Context (language use), Astrophysics, law.invention, Telescope, Optics, law, instrumentation: high angular resolution, Adaptive optics, Coronagraph, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Wavefront, methods: statistical, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, techniques: high angular resolution, Astronomy and Astrophysics, telescopes, Cophasing, Space and Planetary Science, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Context: The detection and characterization of Earth-like exoplanets (exoEarths) from space requires exquisite wavefront stability at contrast levels of $10^{-10}$. On segmented telescopes in particular, aberrations induced by cophasing errors lead to a light leakage through the coronagraph, deteriorating the imaging performance. These need to be limited in order to facilitate the direct imaging of exoEarths. Aims: We perform a laboratory validation of an analytical tolerancing model that allows us to determine wavefront error requirements in the $10^{-6} - 10^{-8}$ contrast regime, for a segmented pupil with a classical Lyot coronagraph. We intend to compare the results to simulations, and we aim to establish an error budget for the segmented mirror on the High-contrast imager for Complex Aperture Telescopes (HiCAT) testbed. Methods: We use the Pair-based Analytical model for Segmented Telescope Imaging from Space (PASTIS) to measure a contrast influence matrix of a real high contrast instrument, and use an analytical model inversion to calculate per-segment wavefront error tolerances. We validate these tolerances on the HiCAT testbed by measuring the contrast response of segmented mirror states that follow these requirements. Results: The experimentally measured optical influence matrix is successfully measured on the HiCAT testbed, and we derive individual segment tolerances from it that correctly yield the targeted contrast levels. Further, the analytical expressions that predict a contrast mean and variance from a given segment covariance matrix are confirmed experimentally., Comment: 16 pages, 16 figures, accepted for publication in A&A
Published: 2022

18. Three-sided pyramid wavefront sensor, part 1: simulations and analysis for astronomical adaptive optics

Author: Jared R. Males, Joseph Long, Lauren Schatz, Johanan L. Codona, Michael Hart, Thierry Fusco, Pierre Janin-Potiron, Robert Johnson, Olivier Fauvarque, Jean-François Sauvage, Vincent Chambouleyron, Carlos Correia, Benoit Neichel, Mala Mateen, Wyant College of Optical Sciences [University of Arizona], University of Arizona, Steward Observatory, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Hart Scientific Consulting International LLC, Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), Air Force Research Laboratory (AFRL), United States Air Force (USAF), ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: High contrast imaging, high contrast imaging, Computer science, Segmented mirror, 01 natural sciences, Deformable mirror, adaptive optics, 010309 optics, [SPI]Engineering Sciences [physics], Giant Magellan Telescope, Optics, 0103 physical sciences, Adaptive optics, 010303 astronomy & astrophysics, Instrumentation, Wavefront sensing, Wavefront, instrumentation, [PHYS]Physics [physics], business.industry, Mechanical Engineering, Strehl ratio, Astronomy and Astrophysics, Wavefront sensor, simulation, Electronic, Optical and Magnetic Materials, Space and Planetary Science, Control and Systems Engineering, wavefront sensing, business, Thirty Meter Telescope, Simulation
Abstract: International audience; The Giant Segmented Mirror Telescopes (GSMTs) including the Giant Magellan Telescope (GMT), the Thirty Meter Telescope (TMT), and the European Extremely Large Telescope (E-ELT), all have extreme adaptive optics (ExAO) instruments planned that will use pyramid wavefront sensors (PWFS). The ExAO instruments all have common features: a high-actuator-count deformable mirror running at extreme speeds (>1 kHz); a high-performance wavefront sensor (WFS); and a high-contrast coronagraph. ExAO WFS performance is currently limited by the need for high spatial sampling of the wavefront which requires large detectors. For ExAO instruments for the next generation of telescopes, alternative architectures of WFS are under consideration because there is a trade-off between detector size, speed, and noise that reduces the performance of GSMT-ExAO wavefront control. One option under consideration for a GSMT-ExAO wavefront sensor is a three-sided PWFS (3PWFS). The 3PWFS creates three copies of the telescope pupil for wavefront sensing, compared to the conventional four-sided PWFS (4PWFS), which uses four pupils. The 3PWFS uses fewer detector pixels than the 4PWFS and should therefore be less sensitive to read noise. Here we develop a mathematical formalism based on the diffraction theory description of the Foucault knife-edge test that predicts the intensity pattern after the PWFS. Our formalism allows us to calculate the intensity in the pupil images formed by the PWFS in the presence of phase errors corresponding to arbitrary Fourier modes. We use these results to motivate how we process signals from a 3PWFS. We compare the raw intensity (RI) method, and derive the Slopes Maps (SM) calculation for the 3PWFS, which combines the three pupil images of the 3PWFS to obtain the X and Y slopes of the wavefront. We then use the Object Oriented MATLAB Adaptive Optics toolbox (OOMAO) to simulate an end-to-end model of an AO system using a PWFS with modulation and compare the performance of the 3PWFS to the 4PWFS. In the case of a low read noise detector, the Strehl ratios of the 3PWFS and 4PWFS are within 0.01. When we included higher read noise in the simulation, we found a Strehl ratio gain of 0.036 for the 3PWFS using RI over the 4PWFS using SM at a stellar magnitude of 10. At the same magnitude, the 4PWFS RI also outperformed the 4PWFS SM, but the gain was only 0.012 Strehl. This is significant because 4PWFS using SM is how the PWFS is conventionally used for AO wavefront sensing. We have found that the 3PWFS is a viable WFS that can fully reconstruct a wavefront and produce a stable closed-loop with correction comparable to that of a 4PWFS, with modestly better performance for high read-noise detectors.
Published: 2021

19. Optical system with a curved detector for wide-field high-resolution cortical imaging at meso-scale

Author: Isabelle Racicot, Joel Baurberg, Eduard Muslimov, Jean-François Sauvage, Marc Ferrari, Kevin Blaize, Xavier Degiovanni, Frédéric Chavane, Institut de Neurosciences de la Timone (INT), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), NOVA Optical IR Instrumentation Group, Kazan National Research Technical University, DOTA, ONERA [Salon], ONERA, and European Project: 777222
Subjects: Physics, Curved detector, Mesoscopic physics, Image quality, business.industry, Gaussian, Detector, Field of view, Curvature, neuroscience, symbols.namesake, large field of view, Optics, cortical imaging, Temporal resolution, symbols, [SDV.NEU]Life Sciences [q-bio]/Neurons and Cognition [q-bio.NC], Focus (optics), business
Abstract: International audience; Optical imaging techniques such as voltage-sensitive dye imaging and intrinsic imaging allow for the recording of neuronal activity at high spatio-temporal scales over a large field of view 1 , 2 revealing some mesoscopic scale dynamics such as propagating waves 3. 4 In practice however, the achievable image quality deteriorates significantly away from the point of best focus due to the curvature of the brain, which fundamentally limits the spatial extent of the cortex that can be studied through a single image. To improve the field of view achievable by optical imaging, we developed a new optical system adapted to the curvature of the non-human primate brain in study. This is achieved by using a curved detector in combination with an appropriate optical system of double Gaussian and aspherical lenses. Furthermore, to ensure a uniform and reliable illumination of the cortex, we have designed and built a new illumination system consisting of a ring of LEDs at four different wavebands. This static solution will enable imaging for the first time neuronal activity over a very large field of view (15-20mm) with high spatial and temporal resolution. Preliminary results show a significant increase of the area in focus of a spherical object imaged through the custom optics compared with the standard neuronal imaging optics.
Published: 2021

20. Analyse du budget d'erreur pour la détection et l'imagerie directe d'exoplanètes par coronographie avec les miroirs déformables du telescope spatial Nancy Grace Roman

Author: David Bourgeois, Iva Laginja, and Jean-François Sauvage
Subjects: Exoplanètes, Imagerie directe, Coronographie
Abstract: The search for exoplanets touches on many different fields in astronomy, optics and instrumen- tation. During my internship at Laboratoire d’Astrophysique de Marseille (LAM), and through- out this document, we are exploring direct imaging techniques for the detection and charac- terization of these worlds. This work is based on an introduction to numerical end-to-end simulators, where I have built the “FFTrial" tool and contributed to “webbPSF". The core of this report talks about the coronagraphic tolerancing model ‘Pair-based Analytical model for Segmented Telescope Imaging from Space (PASTIS), which was originally developed for segmented telescopes, and which I worked on extending for applications to continuous de- formable mirrors. This work aims to support technology developments for coronagraphy on space telescopes like James Webb Space Telescope (JWST), Nancy Grace Roman Space Telescope (RST), Habitable Exoplanet Observatory (HabEx) and Large UV/Optical/Infrared Surveyor (LUVOIR). La recherche d’exoplanètes a ouvert de nombreux champs. Durant mon stage au Laboratoire d’Astrophysique de Marseille (LAM) et au travers de ce document, nous nous intéresserons à détecter et caractériser ces dernières via l’imagerie directe. Nous allons parler de simula- teurs numériques d’optique end-to-end (E2E), notamment FFTrial et webbPSF. Nous allons tenter de corriger des aberrations du front d’onde sur des coronographes avec le logiciel Pair- based Analytical model for Segmented Telescope Imaging from Space (PASTIS). Aussi, on changera le mode de génération des matrices d’aberrations co-phasées segmentés par des Deformable Mirror (DM) continue pour faire du Wavefront Error (WFE) budget. Le tout des télescopes spatiaux que nous allons implémenter ou améliorer comme James Webb Space Telescope (JWST),Nancy Grace Roman Space Telescope (RST)
Published: 2021
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21. High-contrast imager for complex aperture telescopes (HiCAT): 7. Dark zone demonstration with fully segmented aperture coronagraph

Author: Scott D. Will, James Noss, Kelsey Glazer, Jaret Prothro, Iva Laginja, Gregory R. Brady, Hari B. Subedi, Peter Petrone, Raphaël Pourcelot, Evelyn McChesney, Laurent Mugnier, Sam Weinstock, Marshall D. Perrin, Heather Olszewski, Ron Shiri, Susan M. Redmond, John G. Hagopian, Matthew Maclay, Bryony Nickson, Leonid Pogorelyuk, Lucie Leboulleux, Meiji Nguyen, Yinzi Xin, Emiel H. Por, Rémi Soummer, Ananya Sahoo, Mamadou N'Diaye, Anand Sivaramakrishnan, Julia Fowler, Nathan Scott, Maggie Kautz, Rebecca Zhang, Laurent Pueyo, Théo Jolivet, Rob Gontrum, Keira Brooks, Jean-François Sauvage, and Thomas Comeau
Subjects: Physics, Wavefront, business.industry, Aperture, Astrophysics::Instrumentation and Methods for Astrophysics, Wavefront sensor, Deformable mirror, law.invention, Telescope, Tilt (optics), Optics, law, Piston (optics), Astrophysics::Earth and Planetary Astrophysics, business, Coronagraph
Abstract: We present recent laboratory results demonstrating high-contrast coronagraphy for future space-based large segmented telescopes such as the Large UV, Optical, IR telescope (LUVOIR) mission concept studied by NASA. The High-contrast Imager for Complex Aperture Telescopes (HiCAT) testbed aims to implement a system-level hardware demonstration for segmented aperture coronagraphs with wavefront control. The telescope hardware simulator employs a segmented deformable mirror with 36 hexagonal segments that can be controlled in piston, tip, and tilt. In addition, two continuous deformable mirrors are used for high-order wavefront sensing and control. The low-order sensing subsystem includes a dedicated tip-tilt stage, a coronagraphic target acquisition camera, and a Zernike wavefront sensor that is used to measure low-order aberration drifts. We explore the performance of a segmented aperture coronagraph both in “static” operations (limited by natural drifts and instabilities) and in “dynamic” operations (in the presence of artificial wavefront drifts added to the deformable mirrors), and discuss the estimation and control strategies used to reach and maintain the dark zone contrast. We summarize experimental results that quantify the performance of the testbed in terms of contrast, inner/outer working angle and bandpass, and analyze limiting factors by comparing against our end-to-end models.
Published: 2021

22. The bright pyramid wavefront sensor

Author: Jean-François Sauvage, Vincent Chambouleyron, Rebecca Jensen-Clem, Benjamin L. Gerard, University of California Observatories, University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Palaiseau], and ONERA-Université Paris-Saclay
Subjects: Wavefront, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Observational error, business.industry, Detector, Linearity, FOS: Physical sciences, Wavefront sensor, Noise (electronics), [SPI]Engineering Sciences [physics], Tilt (optics), Optics, Astrophysics - Instrumentation and Methods for Astrophysics, business, Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Wavefront sensing, Astrophysics - Earth and Planetary Astrophysics
Abstract: Extreme adaptive optics (AO) is crucial for enabling the contrasts needed for ground-based high contrast imaging instruments to detect exoplanets. Pushing exoplanet imaging detection sensitivities towards lower mass, closer separations, and older planets will require upgrading AO wavefront sensors (WFSs) to be more efficient. In particular, future WFS designs will aim to improve a WFS's measurement error (i.e., the wavefront level at which photon noise, detector noise, and/or sky background limits a WFS measurement) and linearity (i.e., the wavefront level, in the absence of photon noise, aliasing, and servo lag, at which an AO loop can close and the corresponding closed-loop residual level). We present one such design here called the bright pyramid WFS (bPWFS), which improves both the linearity and measurement errors as compared to the non-modulated pyramid WFS (PWFS). The bPWFS is a unique design that, unlike other WFSs, doesn't sacrifice measurement error for linearity, potentially enabling this WFS to (a) close the AO loop on open loop turbulence utilising a tip/tilt modulation mirror (i.e., a modulated bPWFS; analogous to the procedure used for the regular modulated PWFS), and (b) reach deeper closed-loop residual wavefront levels (i.e., improving both linearity and measurement error) compared to the regular non-modulated PWFS. The latter approach could be particularly beneficial to enable improved AO performance using the bWFS as a second stage AO WFS. In this paper we will present an AO error budget analysis of the non-modulated bPWFS as well as supporting AO testbed results from the Marseille Astrophysics Laboratory., Comment: submitted proceedings to SPIE SPIE Optical Engineering + Applications 2021, Techniques and Instrumentation for Detection of Exoplanets X
Published: 2021

23. Calibration of residual aberrations in exoplanet imagers with large numbers of degrees of freedom

Author: Philippe Balard, Jérémy Hulin, Marcel Carbillet, Elodie Choquet, Kjetil Dohlen, Gilles Otten, Mamadou N'Diaye, Mona El Morsy, Raphaël Pourcelot, Jean-François Sauvage, Philippe Blanchard, Bastien Rouzé, Alain Abbinanti, Maxime Lopez, Arthur Vigan, A. Caillat, Émilie Robert, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Département Médico-Universitaire APPROCHES, CHU Tenon [AP-HP], Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Joseph Louis LAGRANGE (LAGRANGE), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Zernike polynomials, FOS: Physical sciences, instrumentation: adaptive optics, 01 natural sciences, Deformable mirror, law.invention, 010309 optics, symbols.namesake, Optics, law, instrumentation: high angular resolution, 0103 physical sciences, Adaptive optics, 010303 astronomy & astrophysics, Coronagraph, Instrumentation and Methods for Astrophysics (astro-ph.IM), [PHYS]Physics [physics], Physics, Wavefront, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, techniques: high angular resolution, Astronomy and Astrophysics, Wavefront sensor, Exoplanet, Starlight, [SDU]Sciences of the Universe [physics], Space and Planetary Science, symbols, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Imaging faint objects, such as exoplanets or disks, around nearby stars is extremely challenging because host star images are dominated by the telescope diffraction pattern. Using a coronagraph is an efficient solution for removing diffraction but requires an incoming wavefront with good quality to maximize starlight rejection. On the ground, the most advanced exoplanet imagers use extreme adaptive optics (ExAO) systems that are based on a deformable mirror (DM) with a large number of actuators to efficiently compensate for high-order aberrations and provide diffraction-limited images. While several exoplanet imagers with DMs using ∼1500 actuators are now routinely operating on large telescopes to observe gas giant planets, future systems may require a tenfold increase in the number of degrees of freedom to look for rocky planets. In this paper, we explore wavefront correction with a secondary adaptive optics system that controls a very large number of degrees of freedom that are not corrected by the primary ExAO system. Using Marseille Imaging Testbed for High Contrast (MITHiC), we implement a second stage of adaptive optics with ZELDA, a Zernike wavefront sensor, and a spatial light modulator to compensate for the phase aberrations of the bench downstream residual aberrations from adaptive optics. We demonstrate that their correction up to 137 cycles per pupil with nanometric accuracy is possible, provided there is a simple distortion calibration of the pupil and a moderate wavefront low-pass filtering. We also use ZELDA for a fast compensation of ExAO residuals, showing its promising implementation as a second-stage correction for the observation of rocky planets around nearby stars. Finally, we present images with a classical Lyot coronagraph on MITHiC and validate our ability to reach its theoretical performance with our calibration.
Published: 2021

24. Focal-plane-assisted pyramid wavefront sensor: Enabling frame-by-frame optical gain tracking

Author: Jean-François Sauvage, Benoit Neichel, Vincent Chambouleyron, Thierry Fusco, Olivier Fauvarque, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), This work benefited from the support of the WOLF project ANR-18-CE31-0018 of the French National Research Agency (ANR). It has also been prepared as part of the activities of OPTICON H2020 (2017-2020) Work Package 1 (Calibration and test tools for AO assisted E-ELT instruments). OPTICON is supported by the Horizon 2020 Framework Programme of the European Commission’s (Grant number 730890). Authors are acknowledging the support by the Action Spécifique Haute Résolution Angulaire (ASHRA) of CNRS/INSU co-funded by CNES. Vincent Chambouleyron PhD is co-funded by 'Région Sud' and ONERA, in collaboration with First Light Imaging. Finally, part of this work is supported by the LabEx FOCUS ANR-11-LABX-0013., ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018), European Project: 730890,OPTICON, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Computer science, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, adaptive optics [instrumentation], Tracking (particle physics), 01 natural sciences, 010309 optics, 0103 physical sciences, Computer vision, Pyramid (image processing), Sensitivity (control systems), Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, business.industry, Frame (networking), telescopes, Astronomy and Astrophysics, Wavefront sensor, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cardinal point, Space and Planetary Science, Path (graph theory), Artificial intelligence, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract: Aims. With its high sensitivity, the pyramid wavefront sensor (PyWFS) is becoming an advantageous sensor for astronomical adaptive optics (AO) systems. However, this sensor exhibits significant non-linear behaviours leading to challenging AO control issues. Methods. In order to mitigate these effects, we propose to use in addition to the classical pyramid sensor a focal plane image combined with a convolutive description of the sensor to fast track the PyWFS non-linearities, the so-called optical gains (OG). Results. We show that this additional focal plane imaging path only requires a small fraction of the total flux while representing a robust solution to estimating the PyWFS OG. Finally, we demonstrate the gain that our method brings with specific examples of bootstrapping and handling non-common path aberrations.
Published: 2021

25. Coronagraphic phase diversity through residual turbulence: performance study and experimental validation

Author: Arthur Vigan, Laurent M. Mugnier, Olivier Herscovici-Schiller, Kjetil Dohlen, Jean-François Sauvage, DTIS, ONERA, Université Paris Saclay (COmUE) [Palaiseau], ONERA-Université Paris Saclay (COmUE), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: HAUTE RÉSOLUTION ANGULAIRE, FOS: Physical sciences, METHODS: DATA ANALYSIS, OPTIQUE ADAPTATIVE, Residual, 01 natural sciences, law.invention, 010309 optics, Speckle pattern, Optics, TRAITEMENT IMAGE, law, TECHNIQUES: IMAGE PROCESSING, 0103 physical sciences, INSTRUMENTATION, Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Coronagraph, Wavefront, Physics, business.industry, Astronomy and Astrophysics, Exoplanet, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cardinal point, Space and Planetary Science, TURBULENCE, TECHNIQUES: HIGH ANGULAR RESOLUTION, Astrophysics - Instrumentation and Methods for Astrophysics, business, Quasistatic process, Physics - Optics, Optics (physics.optics)
Abstract: Quasi-static aberrations in coronagraphic systems are the ultimate limitation to the capabilities of exoplanet imagers both ground-based and space-based. These aberrations - which can be due to various causes such as optics alignment or moving optical parts during the observing sequence - create light residuals called speckles in the focal plane that might be mistaken for a planets. For ground-based instruments, the presence of residual turbulent wavefront errors due to partial adaptive optics correction causes an additional difficulty to the challenge of measuring aberrations in the presence of a coronagraph. In this paper, we present an extension of COFFEE, the coronagraphic phase diversity, to the estimation of quasi-static aberrations in the presence of adaptive optics-corrected residual turbulence. We perform realistic numerical simulations to assess the performance that can be expected on an instrument of the current generation. We perform the first experimental validation in the laboratory which demonstrates that quasistatic aberrations can be corrected during the observations by means of coronagraphic phase diversity., Comment: This is a pre-copyedited, author-produced PDF of an article accepted for publication in the Monthly Notices of the Royal Astronomical Society following peer review
Published: 2019

26. Active optics in deployable systems for future earth observation and science missions

Author: Nicolas Tetaz, Laurent M. Mugnier, Ruben Sanchez-Janssen, Frédéric Falzon, David Boban, Christophe Devilliers, Lauriane Galtier, Stephane Vezain, Marc Ferrari, Mamadou N'Diaye, Aurélien Suau, Noah Schwartz, Jean-François Sauvage, Ludovic Canas, Pascal Hallibert, Laurent Perrona, Guillaume Butel, Stéphanie Behar-Lafenetre, Jérôme Demilly, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Thales Alenia Space [Toulouse] (TAS), THALES [France], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA [Salon], ONERA, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), and The authors gratefully acknowledge support for the work provided by the European Space Agency under contract number 4000125154/18/NL/AR/ig 'ACTIVE OPTICS IN DEPLOYABLE SYSTEMS FOR FUTURE EO AND SCIENCE MISSIONS'.
Subjects: Earth observation, Computer science, Deployable mirror, High resolution, 02 engineering and technology, 01 natural sciences, Positioning mechanism, law.invention, 010309 optics, Entrance pupil, Telescope, law, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Mechanical design, System level, ComputingMilieux_MISCELLANEOUS, [PHYS]Physics [physics], Segmented mirror, Active optics, Wave front sensor, [SDU]Sciences of the Universe [physics], Geostationary orbit, Systems engineering, 020201 artificial intelligence & image processing, Deformable mirror
Abstract: International audience; This paper describes the outcomes of a study funded by the European Space Agency aimed at identifying the technical challenges and trade-offs at the system level, performing preliminary designs of an active correction loop for large deployable telescopes, and defining technological roadmaps for the development of the active correction loop for the selected designs. This study has targeted two very different application cases, one for High Resolution Earth Observation from Geostationary orbit (called GeoHR, with a 4m diameter entrance pupil) and one for Science missions requiring very large telescopes (with a up to 18 m diameter entrance pupil) with high-contrast imaging capabilities for exo-Earth observations and characterization. For both application cases, this paper first summarizes the mission objectives and constraints that have influence on the telescope designs. It then presents the high-level trade-offs that have been led and the optical and mechanical design that have been developed, including the deployable aspects. Finally, the performance assessment is presented, and is the basis for the justification of an active optics correction chain, with a preliminary set of requirements for typical components of the system. The presentation is concluded with proposed technological roadmaps that aim to allow the development of the building blocks on which the next generation instruments will be able to rely on.
Published: 2021

27. Direct imaging and spectroscopy of exoplanets with the ELT/HARMONI high-contrast module

Author: M. Houllé, Jean-François Sauvage, Gilles Otten, Elodie Choquet, Mark W. Phillips, Christoph Mordasini, Noah Schwartz, Isabelle Baraffe, Alexis Carlotti, Alexandre Emsenhuber, Faustine Cantalloube, Arthur Vigan, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, School of Physics and Astronomy [Exeter], University of Exeter, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Bern, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Max Planck Institute for Astronomy (MPIA), NASA GODDARD INSTITUTE FOR SPACE STUDIES NEW YORK USA, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Langages HUmanités Médiations Apprentissages Interactions Numérique (LHUMAIN), Université Paul-Valéry - Montpellier 3 (UPVM), DOTA, ONERA [Salon], ONERA, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Center for Space and Habitability (CSH), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: planets and satellites: detection, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 530 Physics, Instrumentation, FOS: Physical sciences, Astrophysics, 7. Clean energy, law.invention, Telescope, Integral field spectrograph, instrumentation: high angular resolution, Planet, law, Extremely Large Telescope, infrared: planetary systems, Adaptive optics, Spectroscopy, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 520 Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Exoplanet, techniques: imaging spectroscopy, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Combining high-contrast imaging with medium-resolution spectroscopy has been shown to significantly boost the direct detection of exoplanets. HARMONI, one of the first-light instruments to be mounted on ESO's ELT, will be equipped with a single-conjugated adaptive optics system to reach the diffraction limit of the ELT in H and K bands, a high-contrast module dedicated to exoplanet imaging, and a medium-resolution (up to R = 17 000) optical and near-infrared integral field spectrograph. Combined together, these systems will provide unprecedented contrast limits at separations between 50 and 400 mas. In this paper, we estimate the capabilities of the HARMONI high-contrast module for the direct detection of young giant exoplanets. We use an end-to-end model of the instrument to simulate observations based on realistic observing scenarios and conditions. We analyze these data with the so-called "molecule mapping" technique combined to a matched-filter approach, in order to disentangle the companions from the host star and tellurics, and increase the S/N of the planetary signal. We detect planets above 5-sigma at contrasts up to 16 mag and separations down to 75 mas in several spectral configurations of the instrument. We show that molecule mapping allows the detection of companions up to 2.5 mag fainter compared to state-of-the-art high-contrast imaging techniques based on angular differential imaging. We also demonstrate that the performance is not strongly affected by the spectral type of the host star, and that we reach close sensitivities for the best three quartiles of observing conditions at Armazones, which means that HARMONI could be used in near-critical observations during 60 to 70% of telescope time at the ELT. Finally, we simulate planets from population synthesis models to further explore the parameter space that HARMONI and its high-contrast module will soon open., Accepted for publication in A&A (14 pages, 9 figures)
Published: 2021

28. Variation on a Zernike wavefront sensor theme: Optimal use of photons

Author: Thierry Fusco, Jean-François Sauvage, Olivier Fauvarque, Kjetil Dohlen, Arthur Vigan, Mamadou N'Diaye, Nicolas Levraud, Benoit Neichel, Vincent Chambouleyron, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), This work benefited from the support of the WOLF project ANR-18-CE31-0018 of the French National Research Agency (ANR). It has also been prepared as part of the activities of OPTICON H2020 (2017–2020) Work Package 1 (Calibration and test tools for AO assisted E-ELT instruments). OPTICON is supported by the Horizon 2020 Framework Programme of the European Commission’s (Grant number 730890). Authors are acknowledging the support by the Action Spécifique Haute Résolution Angulaire (ASHRA) of CNRS/INSU co-funded by CNES. Vincent Chambouleyron PhD is co-funded by 'Région Sud' and ONERA, in collaboration with First Light Imaging. AV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 757561). Finally, part of this work is supported by the LabEx FOCUS ANR11-LABX-0013, and received the support of Action Spécifique Haute Résolution Angulaire ASHRA., ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018), and European Project: 730890,OPTICON
Subjects: Zernike polynomials, Phase (waves), FOS: Physical sciences, Astrophysics, adaptive optics [instrumentation], 01 natural sciences, 010309 optics, symbols.namesake, Optics, 0103 physical sciences, Sensitivity (control systems), Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Wavefront, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Dynamic range, telescopes, Astronomy and Astrophysics, Wavefront sensor, Wavelength, Cardinal point, Space and Planetary Science, symbols, business, Astrophysics - Instrumentation and Methods for Astrophysics, Optics (physics.optics), Physics - Optics
Abstract: Aims. The Zernike wavefront sensor (ZWFS) is a concept belonging to the wide class of Fourier-filtering wavefront sensors (FFWFSs). The ZWFS is known for its extremely high sensitivity and low dynamic range, which makes it a unique sensor for second stage adaptive optics systems or quasi-static aberration calibration sensors. This sensor is composed of a focal plane mask made of a phase shifting dot that is fully described by two parameters: its diameter and depth. We aim to improve the performance of this sensor by changing the diameter of its phase shifting dot. Methods. We begin with a general theoretical framework, providing an analytical description of the FFWFS properties. We then predict the expected ZWFS sensitivity for different configurations of dot diameters and depths. The analytical predictions are then validated with end-to-end simulations. From this, we propose a variation of the classical ZWFS shape that exhibits extremely appealing properties. Results. We show that the ZWFS sensitivity can be optimized by modifying the dot diameter and it can even reach the optimal theoretical limit, though with the trade-off of low spatial frequency sensitivity. As an example, we show that a ZWFS with a 2 λ/D dot diameter (where λ is the sensing wavelength and D the telescope diameter), hereafter called a Z2WFS, exhibits a sensitivity twice higher than the classical 1.06 λ/D ZWFS for all the phase spatial components except for tip-tilt modes. Furthermore, this gain in sensitivity does not impact the dynamic range of the sensor, and the Z2WFS exhibits a similar dynamical range as the classical 1.06 λ/D ZWFS. This study opens the path to the conception of a diameter-optimized ZWFS.
Published: 2021
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29. Focal plane wavefront sensing on SUBARU/SCExAO

Author: Aurélie Montmerle-Bonnefois, Frédéric Cassaing, Nemanja Jovanovic, Laurent M. Mugnier, Alison Wong, Vincent Deo, Frans Snik, Sébastien Vievard, Coline Lopez, Michael J. Wilby, Barnaby Norris, Steven P. Bos, Thayne Currie, Christoph U. Keller, Mamadou N'Diaye, Jean-François Sauvage, Nour Skaf, Frantz Martinache, Olivier Guyon, Masen Lamb, Ananya Sahoo, Kelsey Miller, Julien Lozi, National Astronomical Observatory of Japan (NAOJ), Astrobiology Center of Nins, DTIS, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, California Institute of Technology (CALTECH), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], DOTA, ONERA, Université Paris Saclay [Châtillon], Schreiber, Laura, Schmidt, Dirk, and Vernet, Elise
Subjects: High contrast imaging, LOW WIND EFFECT, FOS: Physical sciences, 01 natural sciences, 010309 optics, [SPI]Engineering Sciences [physics], Optics, Wind effect, 0103 physical sciences, Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Focal plane wavefront sensing, Physics, Wavefront, [PHYS]Physics [physics], [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], business.industry, CORONOGRAPHY, Detector, Spiders, SCEXAO, Cardinal point, CORONAGRAPHY, Adaptive optics systems, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Focal plane wavefront sensing is an elegant solution for wavefront sensing since near-focal images of any source taken by a detector show distortions in the presence of aberrations. Non-Common Path Aberrations and the Low Wind Effect both have the ability to limit the achievable contrast of the finest coronagraphs coupled with the best extreme adaptive optics systems. To correct for these aberrations, the Subaru Coronagraphic Extreme Adaptive Optics instrument hosts many focal plane wavefront sensors using detectors as close to the science detector as possible. We present seven of them and compare their implementation and efficiency on SCExAO. This work will be critical for wavefront sensing on next generation of extremely large telescopes that might present similar limitations., Comment: SPIE proceeding : Astronomical Telescopes + Instrumentation 2020. arXiv admin note: text overlap with arXiv:1912.10179
Published: 2020

30. Injecting pupil binary intensity map into the laboratory adaptive optics bench using phase-only LCoS-SLM device

Author: Kacem El Hadi, Thierry Fusco, Jean-François Sauvage, P. Janin-Potiron, Jean-Pierre Veran, David R. Andersen, Mojtaba Taheri, Benoit Neichel, Vincent Chambouleyron, University of Victoria [Canada] (UVIC), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), National Research Council of Canada (NRC), ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018), Schmidt, Dirk, Schreiber, Laura, and Vernet, Elise
Subjects: Optical benches, Scale (ratio), Computer science, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spatial light modulators, Device simulation, Phase (waves), Binary number, Optical instrument design, law.invention, Telescope, [SPI]Engineering Sciences [physics], Optics, law, Binary data, Large telescopes, Extremely large telescope, Adaptive optics, spatial light modulator, ComputingMilieux_MISCELLANEOUS, [PHYS]Physics [physics], Spatial light modulator, business.industry, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Liquid crystal on silicon, focal-plane filtering, Manufacturing, business, intensity modulation, Telescopes
Abstract: Laboratory Adaptive Optics (AO) benches are the backbone of experimental testing and verification of new AO designs and architectures. These testbeds are particularly important when exploring unknown factors in the development of new instruments and facilities like future extremely large telescope AO systems. One of the key elements for simulating the performance of such systems in a smaller scale laboratory environment is the ability of projecting the precise intensity mask on the pupil plane. This mask often has binary (black or transparent/reflective) patterns that mimic the secondary obscuration and spider design of the telescope. Precise implementation of such intensity masks on the bench is important since studying effects such as “island/petaling effect” are critically dependent on the correct down-scaling and precise representation of the spider structure. Using a physical mask for such an application is very difficult since manufacturing and installing such fine structure pieces are difficult and hard to use. It is also necessary to build a new physical mask for each telescope system or scale that is desired for the experiment. In this paper, we introduce two methods of using a phase only Liquid Crystal on Silicon Spatial Light Modulator (LCoS-SLM) device as an alternative option to precisely and relatively easily inject the custom intensity mask into an optical bench. By implementing these methods on the LOOPS bench AO facilities of the LAM, we demonstrated that the contrast produced by both methods could be better than 2% (dark/bright ratio), which is sufficient for representing pupil obscuration in the majority of applications. We also show that by using one of these methods, it is possible to inject phase and binary intensity mask simultaneously which could greatly increase the versatility and ease of use of an experimental AO setup., Adaptive Optics Systems VII, December 14-18, 2020, Online Only, United States, Series: Proceedings of SPIE
Published: 2020

31. HARMONI: first light spectroscopy for the ELT: instrument final design and quantitative performance predictions

Author: Sofia Dimoudi, Jorge Chao Ortiz, Alexandre Jeanneau, Joel Vernet, Eric Daguisé, Adrien Hours, William Bon, Laurence Routledge, Ian Tosh, Eric Stadler, Ana Monreal, Kearn Grisdale, Ruben Sanchez-Janssen, Luis Fernando Rodriguez-Ramos, Jim Lynn, Alvaro Menduina, Angel Alonso Sanchez, Javier Piqueras López, Sylvain Guieu, Aurélien Jarno, Lazar Staykov, Teodora Viera, Joshua Hopgood, Chris Miller, David King, Vanessa Ferraro-Wood, Edgard Renault, Sandi Wilson, Matteo Accardo, James Carruthers, Alberto Estrada Piqueras, Matthieu Guibert, Cyril Petit, Angus Gallie, Zoltan Hubert, William Cochrane, Patricia Fernández Izquierdo, Kenny Campbell, Afrodisio Vega Moreno, Thierry Fusco, David Gooding, Patrice Sanchez, Madeline Close, Mark Swinbank, Jose Luis Rasilla, Arthur Vigan, Andrea Melissa Hidalgo, Romain Fétick, Miguel Pereira Santaella, Adam Lowe, Hermine Schnetler, Michael Meyer, E. Joven, Jean-Luc Gach, Yves Magnard, Josh Anderson, Benoit Neichel, Andy Born, José Peñate Castro, Simon L. Morris, José Linares, Kayhan Gültekin, Nicholas Bouché, Naomi Dobson, Chris Evans, John Capone, Jean-François Sauvage, Yolanda Martín Hernando, Miguel A. Cagigas, Jean-Emmanuel Migniau, Lynn Ritchie, Noah Schwartz, Didier Boudon, Ian Bryson, Alejandro Crespo, Neil Campbell, Jose Miguel Delgado, Alexis Carlotti, Johan Richard, Benoit Epinat, Matthew J. Townson, Stuart Watt, Charlotte Bond, Monica Valluri, Martin Black, Ellis Elliott, Pascal Vola, Elvio Hernandez Suarez, Miriam García García, Magali Loupias, Kacem El-Hadi, Fraser Clarke, John Murray, Matthias Tecza, Patrick Smith, Domingo Avarez Mendez, Leander Mehrgan, Nick Cann, Kjetil Dohlen, Frédéric Gonté, Karen Disseau, Lisa Bardou, Michael J. Booth, David Montgomery, Dave Melotte, Laurent Jocou, Nicola Vedrenne, Florence Laurent, Ana Belén. Fragoso López, Carlos Correia, Tom Louth, William Humphreys, Felipe Pedreros, David Henry, James Kariuki, David Le Mignant, Patrick Rabou, Elizabeth George, Olivier Beltramo-Martin, Sebastian Egner, Olivier Groussin, C. B. Lim, S. Rousseau, Myriam Rodrigues, Jean-Jacques Correia, Martyn Wells, Marc Llored, Thierry Contini, Ralf Conzelmann, Thibaut Moulin, Tea Seitis, Taha Bagci, Joel Le Merrer, Jeremy Blaizot, Oscar A. Gonzalez, Anne Bonnefoi, A. Remillieux, Diane Chapuis, Tim Morris, Derek Ives, Niranjan Thatte, Dimitra Rigopoulou, Roy Preece, Elodie Choquet, Laure Piqueras, Maria Begoña. Garcia-Lorenzo, Fabrice Pancher, Alain Delboulbe, Marie Larrieu, Battaglia Giuseppina, William Ceria, Mario Mateo, Michele Cappellari, Celine Peroux, Rishi Deshmukh, Arlette Pécontal-Rousset, Santiago Arribas, Roberto López, Joel Harman, Norman O'Malley, E. Mueller, Issa Jaafar, Zeynep Ozer, Kieran O'Brien, Anne Costille, Franck Ducret, Yan Fantei-Caujolle, Eddy Younger, Ian Lewis, Marc Dubbledam, Rafael Rebolo, Munadi Ahmad, Evencio Mediavilla, Daniel Lecron, DOTA, ONERA, Université Paris Saclay [Châtillon], and ONERA-Université Paris-Saclay
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Computer science, Integration testing, First light, 01 natural sciences, 010309 optics, Integral field spectrograph, 0103 physical sciences, Systems engineering, Milestone (project management), Extremely Large Telescope, Adaptive optics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Design review
Abstract: HARMONI is the adaptive optics assisted, near-infrared and visible light integral field spectrograph for the Extremely Large Telescope (ELT). A first light instrument, it provides the work-horse spectroscopic capability for the ELT. As the project approaches its Final Design Review milestone, the design of the instrument is being finalized, and the plans for assembly, integration and testing are being detailed. We present an overview of the instrument's capabilities from a user perspective, provide a summary of the instrument's design, including plans for operations and calibrations, and provide a brief glimpse of the predicted performance for a specific observing scenario. The paper also provides some details of the consortium composition and its evolution since the project commenced in 2015.
Published: 2020

32. Estimating low-order aberrations through a Lyot coronagraph with a Zernike wavefront sensor for exoplanet imaging

Author: James Noss, Marcel Carbillet, Arthur Vigan, Kjetil Dohlen, Julia Fowler, Emiel H. Por, Iva Laginja, Greg Brady, Raphaël Pourcelot, Matthew Maclay, Jean-François Sauvage, Scott D. Will, Pete Petrone, Mamadou N'Diaye, Marshall D. Perrin, Rémi Soummer, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Space Telescope Science Institute (STSci), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, SigmaSpace Corporation [Lanham, MD], Leiden Observatory [Leiden], Universiteit Leiden [Leiden], The Institute of Optics, University of Rochester, University of Rochester [USA], NASA Goddard Space Flight Center (GSFC), and Universiteit Leiden
Subjects: Zernike polynomials, FOS: Physical sciences, ZWFS - Zernike wavefront sensor, 01 natural sciences, law.invention, 010309 optics, Telescope, Primary mirror, symbols.namesake, [SPI]Engineering Sciences [physics], Optics, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Coronagraph, Wavefront, Physics, [PHYS]Physics [physics], business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Wavefront sensor, Low-order wavefront sensor, Exoplanet, Starlight, High-contrast imaging, 13. Climate action, symbols, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business, Coronagraphy
Abstract: Imaging exo-Earths is an exciting but challenging task because of the 10^-10 contrast ratio between these planets and their host star at separations narrower than 100 mas. Large segmented aperture space telescopes enable the sensitivity needed to observe a large number of planets. Combined with coronagraphs with wavefront control, they present a promising avenue to generate a high-contrast region in the image of an observed star. Another key aspect is the required stability in telescope pointing, focusing, and co-phasing of the segments of the telescope primary mirror for long-exposure observations of rocky planets for several hours to a few days. These wavefront errors should be stable down to a few tens of picometers RMS, requiring a permanent active correction of these errors during the observing sequence. To calibrate these pointing errors and other critical low-order aberrations, we propose a wavefront sensing path based on Zernike phase-contrast methods to analyze the starlight that is filtered out by the coronagraph at the telescope focus. In this work we present the analytical retrieval of the incoming low order aberrations in the starlight beam that is filtered out by an Apodized Pupil Lyot Coronagraph, one of the leading coronagraph types for starlight suppression. We implement this approach numerically for the active control of these aberrations and present an application with our first experimental results on the High-contrast imager for Complex Aperture Telescopes (HiCAT) testbed, the STScI testbed for Earth-twin observations with future large space observatories, such as LUVOIR and HabEx, two NASA flagship mission concepts., Comment: Presented at SPIE Astronomical Telescopes + Instrumentation 2020
Published: 2020

33. Operational forecast of the PSF figures of merit

Author: Alessio Turchi, Julien Milli, Enrico Pinna, Thierry Fusco, Olivier Beltramo-Martin, Guido Agapito, Benoit Neichel, Elena Masciadri, Jean-François Sauvage, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, ITA, FRA, and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)
Subjects: Computer science, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Atmospheric model, computer.software_genre, 01 natural sciences, adaptive optics, 010309 optics, Atmosphere, [SPI]Engineering Sciences [physics], 0103 physical sciences, Figure of merit, turbulence forecast, Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Remote sensing, [PHYS]Physics [physics], turbulence, Strehl ratio, numerical modelling, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Simulation software, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Full width at half maximum, Upgrade, machine learning, Astrophysics - Instrumentation and Methods for Astrophysics, computer
Abstract: The optimization and scheduling of scientific observations done with instrumentation supported by adaptive optics could greatly benefit from the forecast of PSF figures of merit (FWHM, Strehl Ratio, Encircle Energy and contrast), that depend on the AO instrument, the scientific target and turbulence conditions during the observing night. In this contribution we explore the the possibility to forecast a few among the most useful PSF figures of merit (SR and FWHM). To achieve this goal, we use the optical turbulence forecasted by the mesoscale atmospheric model Astro-Meso-NH on a short timescale as an input for PSF simulation software developed and tailored for specific AO instruments. A preliminary validation will be performed by comparing the results with on-sky measured PSF figures of merit obtained on specific targets using the SCAO systems SOUL (FLAO upgrade) feeding the camera LUCI at LBT and SAXO, the extreme SCAO system feeding the high resolution SPHERE instrument at VLT. This study will pave the way to the implementation of an operational forecasts of such a figure of merits on the base of existing operational forecast system of the atmosphere (turbulence and atmospheric parameters). In this contribution we focus our attention on the forecast of the PSF on-axis., Comment: 9 pages, 3 figures, 2 tables
Published: 2020

34. High-resolution deployable CubeSat prototype

Author: Alex Ward, Donald MacLeod, Noah Schwartz, Maria Milanova, Katherine Morris, William Brzozowski, David Lunney, Jean-François Sauvage, Zeshan Ali, Stephen Todd, UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, and Razorbill Instruments Ltd
Subjects: Deployable optics, Aperture, 02 engineering and technology, 01 natural sciences, law.invention, 010309 optics, Telescope, Primary mirror, [SPI]Engineering Sciences [physics], Optics, law, 0103 physical sciences, CubeSat, Wavefront sensing, Physics, [PHYS]Physics [physics], business.industry, Cassegrain reflector, 021001 nanoscience & nanotechnology, Cophasing, Tilt (optics), Co-phasing, 0210 nano-technology, Secondary mirror, business, Active optics
Abstract: International audience; The volume available on-board small satellites limit the optical aperture to a few centimetres, which limits the Ground-Sampling Distance (GSD) in the visible to approximately 3 m at 500 km. We present the latest development of a laboratory demonstrator for a deployable telescope that will triple the achievable ground resolution and quadruple the photometric capability from a CubeSat imager. In this paper, we present the overall opto-mechanical design of a Cassegrain telescope with a segmented primary mirror with a 30 cm baseline. The segments are folded for launch and unfold in space. To enable diffraction-limited imaging, piston, tip, and tilt (PTT) on each of the mirror segments should be below 12 nm RMS. The key challenge is to ensure phasing, and this precision level will require an active phasing stage. We present laboratory results of deployment and active phasing of the primary mirror segments. The initial deployment is performed using shaped memory alloy that deploy mirror segments. We demonstrate a repeatability below ±4.5 µm, enabling the four PSFs (one for each mirror segment) to be imaged on the detector simultaneously. An alignment step using compact and calibrated capacitive sensors allows for a control of the mirror positions in PTT below the wavelength. Finally, we investigate the sensitivity of misalignments of a deployable secondary mirror and show that it is well within reach of the technology developed in this study.
Published: 2020

35. Laboratory demonstration of focal plane wavefront sensing using phase diversity: a way to tackle the problem of NCPA in SHARK-NIR

Author: Maria Bergomi, Valentina Viotto, Federico Biondi, Daniele Vassallo, Thierry Fusco, Andrea Baruffolo, Marco De Pascale, Jacopo Farinato, Davide Greggio, Elena Carolo, Moritz Plenz, Kalyan Radhakrishnan, Jean-François Sauvage, Luca Marafatto, and Gabriele Umbriaco
Subjects: Wavefront, Amplitude, Cardinal point, Channel (digital image), business.industry, Computer science, Path (graph theory), Context (language use), Large Binocular Telescope, Computer vision, Artificial intelligence, Differential (infinitesimal), business
Abstract: Phase diversity is a wavefront sensing technique that makes use of images in the scientific channel to derive the instrumental aberrations. Two images of whatever object are required, with a well-calibrated differential aberration (typically a pure defocus) between the two. We present here the laboratory demonstration of this concept in the specific context of SHARK-NIR, the new-generation high contrast imager for the Large Binocular Telescope. We investigated the behavior of the sensor in presence of several aberrations of variable amplitude and we optimized the retrieval algorithm parameters by comparing the results with the ones of a Shack-Hartmann sensor. We illustrate the challenges and the perspectives of this technique in view of its application to sense non-common path aberrations in SHARK-NIR.
Published: 2020

36. First error budget of a deployable CubeSat telescope

Author: Sébastien Vievard, Jean-François Sauvage, Marie-Thérèse Velluet, Aurélie Bonnefois, Carlos Correia, Noah Schwartz, Iva Laginja, J. C. Krapez, Thierry Fusco, V. Michau, Marc Ferrari, Frédéric Cassaing, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), National Astronomical Observatory of Japan (NAOJ), Space ODT - Optical Deblurring Technologies, DTIS, ONERA, Université Paris Saclay [Palaiseau], DOTA, ONERA [Salon], ONERA, and Space Telescope Science Institute (STSci)
Subjects: Aperture, Computer science, High-resolution imaging, Imagerie à haute résolution, 02 engineering and technology, Haute résolution angulaire, 01 natural sciences, law.invention, 010309 optics, Telescope, Primary mirror, [SPI]Engineering Sciences [physics], High angular resolution, Low earth orbit, law, 0103 physical sciences, CubeSat, Angular resolution, Aerospace engineering, Active space optics, [PHYS]Physics [physics], Earth observation, Payload, business.industry, Optique active spatiale, Active optics, 021001 nanoscience & nanotechnology, Cophasing, Satellite, 0210 nano-technology, business, Observation de la Terre
Abstract: International audience; The volume available on-board small satellites limit the optical aperture to a few centimetres, which limits the Ground- Sampling Distance (GSD) in the visible to approximately 3 m at 500 km. We present a performance analysis of the concept of a deployable CubeSat telescope. This payload will allow a tripling of the ground resolution achievable from a CubeSat imager, hence allowing very high resolution imaging from Low Earth Orbit (LEO). The project combines precision opto-mechanical deployment and cophasing of the mirrors segments using active optics. The payload has the potential of becoming a new off-the-shelf standardised system to be proposed for all high angular resolution imaging missions using CubeSats or similar nanosats. Ultimately, this technology will develop new instrumentation and technology for small satellite platforms with a primary mirror size equal or larger than 30 cm. In this paper, we present the breakdown of the different error sources that may affect the final optical quality and propose cophasing strategies. We show that the piston, tip and tilt aberrations may need to be as small as 15 nm RMS to allow for diffraction-limited imaging. By taking a co-conception approach, i.e. by taking into account the post-processing capability such as deconvolution, we believe these constraints may be somewhat released. Finally, we show numerical simulation of different solutions allowing the aberrations of the primary mirror segments.; Le volume disponible à bord d'un CubeSat limite la taille de l'ouverture optique à quelques centimètres tout au plus, ce qui limite la résolution au sol atteignable à quelques 3m depuis une orbite basse de 500km. Nous présentons une analyse de performance d'un concept de télescope déployable pour CubeSat. Cette charge utile permettra de tripler la résolution au sol atteignable par un imageur CubeSat, délivrant ainsi une imagerie à très haute résolution depuis une Orbite basse (LEO). Le projet combine le déploiement à grande précision du miroir primaire ainsi que le cophasage de ses pétales en utilisant l'optique active. La charge utile a le potentiel de devenir un nouveau composant sur étagère standardisé, proposé par les concepteurs de CubeSat, pour toutes les missions d'imagerie utilisant les CubeSat ou nanosat. In fine, cette technologie permettra de développer une instrumentation et technologie nouvelles pour les petites plate-formes spatiales, avec un télescope de 30cm. Dans ce papier, nous présentons les spécifications et les différents contributeurs du budget d'erreur qui assurent la performance optique finale. Nous montrons que les erreurs de cophasage en piston, tip et tilt doivent être de l'ordre de quelques dizaines de nanomètres pour assurer la plus haute qualité possible. En utilisant une approche de co-conception, c'est à dire en prenant en compte le post-traitement comme la déconvolution, nous montrons que ces contraintes peuvent être relâchées. Finalement, nous montrons par des simulations numériques les méthodes permettant de mesurer les aberrations du miroir primaire.
Published: 2020

37. Predicting contrast sensitivity to segmented aperture misalignment modes for the HiCAT testbed

Author: Keira Brooks, Scott D. Will, Iva Laginja, J. Scott Knight, Jean-François Sauvage, Lucie Leboulleux, Laurent Pueyo, Laura E. Coyle, Laurent M. Mugnier, Marshall D. Perrin, Julia Fowler, James Noss, Rémi Soummer, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Space Telescope Science Institute (STSci), Observatoire de Paris, Université Paris sciences et lettres (PSL), Ball Aerospace and Technologies Corp., The Institute of Optics, University of Rochester, University of Rochester [USA], University of California [Santa Cruz] (UCSC), University of California, Makenzie Lystrup, Marshall D. Perrin, Natalie Batalha, Nicholas Siegler, and Edward C. Tong
Subjects: Aperture, Computer science, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, FOS: Physical sciences, 01 natural sciences, Deformable mirror, law.invention, 010309 optics, Telescope, Error budget, law, 0103 physical sciences, Sensitivity (control systems), Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Coronagraph, Simulation, Segmented telescope, Measure (data warehouse), Wavefront requirements, Testbed, Wavefront sensing and control, Exoplanet, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Upgrade, High-contrast imaging, Wavefront error tolerancing, Astrophysics - Instrumentation and Methods for Astrophysics, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, Cophasing
Abstract: This paper presents the setup for empirical validations of the Pair-based Analytical model for Segmented Telescope Imaging from Space (PASTIS) tolerancing model for segmented coronagraphy. We show the hardware configuration of the High-contrast imager for Complex Aperture Telescopes (HiCAT) testbed on which these experiments will be conducted at an intermediate contrast regime between $10^{-6}$ and $10^{-8}$. We describe the optical performance of the testbed with a classical Lyot coronagraph and describe the recent hardware upgrade to a segmented mode, using an IrisAO segmented deformable mirror. Implementing experiments on HiCAT is made easy through its top-level control infrastructure that uses the same code base to run on the real testbed, or to invoke the optical simulator. The experiments presented in this paper are run on the HiCAT testbed emulator, which makes them ready to be performed on actual hardware. We show results of three experiments with results from the emulator, with the goal to demonstrate PASTIS on hardware next. We measure the testbed PASTIS matrix, and validate the PASTIS analytical propagation model by comparing its contrast predictions to simulator results. We perform the tolerancing analysis on the optical eigenmodes (PASTIS modes) and on independent segments, then validate these results in respective experiments. This work prepares and enables the experimental validation of the analytical segment-based tolerancing model for segmented aperture coronagraphy with the specific application to the HiCAT testbed., Comment: 18 pages, 9 figures, published
Published: 2020

38. Ongoing flyby in the young multiple system UX Tauri

Author: S. Rochat, Myriam Benisty, Yann Boehler, Christian Ginski, Norbert Hubin, Antonio Garufi, Alice Zurlo, R. G. van Holstein, Janis Hagelberg, Nicolás Cuello, M. Villenave, Daniel J. Price, Raffaele Gratton, Anne-Lise Maire, G. van der Plas, Garreth Ruane, S. Chripko, Arthur Vigan, P. Pinilla, H. M. Schmid, François Ménard, Eric Stadler, A. Boccaletti, Th. Henning, J. de Boer, Carsten Dominik, Jean-François Sauvage, Jean-François Gonzalez, Christophe Pinte, Maud Langlois, A. Pavlov, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Leiden Observatory [Leiden], Universiteit Leiden, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), University of Arizona, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Bulgarian Academy of Sciences (BAS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), Low Energy Astrophysics (API, FNWI), Faculty of Science, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Universiteit Leiden [Leiden], École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Semi-major axis, FOS: Physical sciences, stars: pre-main sequence, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, circumstellar matter, 01 natural sciences, 0103 physical sciences, Coming out, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, protoplanetary disks, Astronomy and Astrophysics, Polarization (waves), Position angle, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Circumstellar disk, Stars, Astrophysics - Solar and Stellar Astrophysics, binaries: general, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Scattered light, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present observations of the young multiple system UX Tauri to look for circumstellar disks and for signs of dynamical interactions. We obtained SPHERE/IRDIS deep differential polarization images in the J and H bands. We also used ALMA archival CO data. Large extended spirals are well detected in scattered light coming out of the disk of UX Tau A. The southern spiral forms a bridge between UX Tau A and C. These spirals, including the bridge connecting the two stars, all have a CO (3-2) counterpart seen by ALMA. The disk of UX Tau C is detected in scattered light. It is much smaller than the disk of UX Tau A and has a major axis along a different position angle, suggesting a misalignment. We performed PHANTOM SPH hydrodynamical models to interpret the data. The scattered light spirals, CO emission spirals and velocity patterns of the rotating disks, and the compactness of the disk of UX Tau C all point to a scenario in which UX Tau A has been perturbed very recently (about 1000 years) by the close passage of UX Tau C., Comment: Accepted for publication in Astronomy & Astrophysics Letters. (8pages, 8 figures). 2 movies will be available on-line
Published: 2020

39. Performance limits of adaptive-optics/high-contrast imagers with pyramid wavefront sensors

Author: Vincent Chambouleyron, Charlotte Z. Bond, Olivier Fauvarque, Carlos M. Correia, Jean-François Sauvage, Thierry Fusco, W.M. Keck Observatory, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], and ONERA-Université Paris-Saclay
Subjects: Physics, Wavefront, Coupling, [PHYS]Physics [physics], Instrumentation: adaptive optics, FOS: Physical sciences, Astronomy and Astrophysics, Atmospheric effects, 01 natural sciences, 010309 optics, Techniques: high angular resolution, [SPI]Engineering Sciences [physics], Space and Planetary Science, Aliasing, 0103 physical sciences, Pyramid (image processing), Chromatic scale, Sensitivity (control systems), Methods: analytical, Adaptive optics, Focus (optics), Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Algorithm, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: Advanced AO systems will likely utilise Pyramid wave-front sensors (PWFS) over the traditional Shack-Hartmann sensor in the quest for increased sensitivity, peak performance and ultimate contrast. Here, we wish to bring knowledge and quantify the PWFS theoretical limits as a means to highlight its properties and use cases. We explore forward models for the PWFS in the spatial-frequency domain for they prove quite useful since a) they emanate directly from physical-optics (Fourier) diffraction theory; b) provide a straightforward path to meaningful error breakdowns, c) allow for reconstruction algorithms with $O (n\,log(n))$ complexity for large-scale systems and d) tie in seamlessly with decoupled (distributed) optimal predictive dynamic control for performance and contrast optimisation. All these aspects are dealt with here. We focus on recent analytical PWFS developments and demonstrate the performance using both analytic and end-to-end simulations. We anchor our estimates with observed on-sky contrast on existing systems and then show very good agreement between analytical and Monte-Carlo estimates for the PWFS. For a potential upgrade of existing high-contrast imagers on 10\,m-class telescopes with visible or near-infrared PWFS, we show under median conditions at Paranal a contrast improvement (limited by chromatic and scintillation effects) of 2x-5x by replacing the wave-front sensor alone at large separations close to the AO control radius where aliasing dominates, and factors in excess of 10x by coupling distributed control with the PWFS over most of the AO control region, from small separations starting with the Inner Working Angle of typically 1-2 $\lambda/D$ to the AO correction edge (here 20 $\lambda/D$)., Comment: 12 pages, 13 figures
Published: 2020

40. Increasing the raw contrast of VLT/SPHERE with the dark hole technique

Author: Julien Milli, Elsa Huby, Anthony Boccaletti, Mamadou N'Diaye, Jean-François Sauvage, Axel Potier, Pierre Baudoz, Arthur Vigan, Zahed Wahhaj, Raphael Galicher, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: media_common.quotation_subject, FOS: Physical sciences, Context (language use), Astrophysics, instrumentation: adaptive optics, 01 natural sciences, law.invention, Telescope, Optics, law, instrumentation: high angular resolution, 0103 physical sciences, Adaptive optics, 010303 astronomy & astrophysics, Coronagraph, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Wavefront, Physics, 010308 nuclear & particles physics, business.industry, Plane (geometry), Astrophysics::Instrumentation and Methods for Astrophysics, techniques: high angular resolution, Astronomy and Astrophysics, Exoplanet, Space and Planetary Science, Sky, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Context. Since 1995 and the first discovery of an exoplanet orbiting a main-sequence star, 4000 exoplanets have been discovered using several techniques. However, only a few of these exoplanets were detected through direct imaging. Indeed, the imaging of circumstellar environments requires high-contrast imaging facilities and accurate control of wavefront aberrations. Ground-based planet imagers such as VLT/SPHERE or Gemini/GPI have already demonstrated great performance. However, their limit of detection is hampered by suboptimal correction of aberrations unseen by adaptive optics (AO). Aims. Instead of focusing on the phase minimization of the pupil plane as in standard AO, we aim to directly minimize the stellar residual light in the SPHERE science camera behind the coronagraph to improve the contrast as close as possible to the inner working angle. Methods. We propose a dark hole (DH) strategy optimized for SPHERE. We used a numerical simulation to predict the global improvement of such a strategy on the overall performance of the instrument for different AO capabilities and particularly in the context of a SPHERE upgrade. Then, we tested our algorithm on the internal source with the AO in closed loop. Results. We demonstrate that our DH strategy can correct for aberrations of phase and amplitude. Moreover, this approach has the ability to strongly reduce the diffraction pattern induced by the telescope pupil and the coronagraph, unlike methods operating at the pupil plane. Our strategy enables us to reach a contrast of 5e-7 at 150 mas from the optical axis in a few minutes using the SPHERE internal source. This experiment establishes the grounds for implementing the algorithm on sky in the near future., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2020

41. On-sky verification of Fast and Furious focal-plane wavefront sensing: Moving forward toward controlling the island effect at Subaru/SCExAO

Author: Christoph U. Keller, Olivier Guyon, Nemanja Jovanovic, Sébastien Vievard, Julien Lozi, Frantz Martinache, Steven P. Bos, Frans Snik, Michael J. Wilby, Barnaby Norris, Jean-François Sauvage, Leiden University, Rapenburg 70, Leiden, 2311 EZ, Netherlands, National Astronomical Observatory of Japan, Subaru Telescope, 650 North Aohoku Place, Hilo, HI 96720, United States, Astrobiology center, National Institutes of Natural sciences, Tokyo, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Leiden Observatory, Leiden University, The Netherlands, National Astronomical Observatory of Japan, Subaru Telescope, 650 North A‘ohoku Place, Hilo, HI 96720, United States, Sydney Astrophotonic Instrumentation Labs, University of Sydney, Australia, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Observatoire de la Cte d’Azur, 96 Boulevard de l’Observatoire, Nice, 06300, France, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, and Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
Subjects: Point spread function, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, 010309 optics, [SPI]Engineering Sciences [physics], Optics, Distortion, 0103 physical sciences, Adaptive optics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Optical path length, instrumentation, [PHYS]Physics [physics], Physics, Wavefront, Earth and Planetary Astrophysics (astro-ph.EP), business.industry, Strehl ratio, Astronomy and Astrophysics, Wavefront sensor, adaptive optics -instrumentation, Space and Planetary Science, business, Astrophysics - Instrumentation and Methods for Astrophysics, high angular resolution, Astrophysics - Earth and Planetary Astrophysics
Abstract: High-contrast imaging (HCI) observations of exoplanets can be limited by the island effect (IE). On the current generation of telescopes, the IE becomes a severe problem when the ground wind speed is below a few meters per second. This is referred to as the low-wind effect (LWE). The LWE severely distorts the point spread function (PSF), significantly lowering the Strehl ratio and degrading the contrast. In this article, we aim to show that the focal-plane wavefront sensing (FPWFS) algorithm, Fast and Furious (F&F), can be used to measure and correct the IE/LWE. We deployed the algorithm on the SCExAO HCI instrument at the Subaru Telescope using the internal near-infrared camera in H-band. We tested F&F with the internal source, and it was deployed on-sky to test its performance with the full end-to-end system and atmospheric turbulence. The performance of the algorithm was evaluated by two metrics based on the PSF quality: 1) the Strehl ratio approximation ($SRA$), and 2) variance of the normalized first Airy ring ($VAR$). Random LWE phase screens with a peak-to-valley wavefront error between 0.4 $��$m and 2 $��$m were all corrected to a $SRA$ $>$90\% and an $VAR\lessapprox0.05$. Furthermore, the on-sky results show that F&F is able to improve the PSF quality during very challenging atmospheric conditions (1.3-1.4'' seeing at 500 nm). Closed-loop tests show that F&F is able to improve the $VAR$ from 0.27 to 0.03 and therefore significantly improve the symmetry of the PSF. Simultaneous observations of the PSF in the {optical} ($��= $ 750 nm, $��=$ 50 nm) show that during these tests we were correcting aberrations common to the optical and NIR paths within SCExAO. Going forward, the algorithm is suitable for incorporation into observing modes, which will enable PSFs of higher quality and stability during science observations., Accepted for publication in A&A. Abstract shortened for arXiv
Published: 2020

42. Compensation des gains optiques d'un capteur à front d'onde pyramidal à l'aide d'un modèle convolutif

Author: P. Janin-Potiron, Jean-François Sauvage, Vincent Chambouleyron, Thierry Fusco, Olivier Fauvarque, Benoit Neichel, Noah Schwartz, Carlos Correia, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), W.M. Keck Observatory, and ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018)
Subjects: Gain optique, Fried parameter, Adaptative optics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Context (language use), Astrophysics, Optical gain, adaptive optics [instrumentation], Residual, 01 natural sciences, 010309 optics, [SPI]Engineering Sciences [physics], Convolutional model, 0103 physical sciences, Optique adaptative, Pyramid (image processing), Sensitivity (control systems), Adaptive optics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Wavefront sensing, Physics, Wavefront, [PHYS]Physics [physics], Astronomy and Astrophysics, Wavefront sensor, Pyramid wave front sensor, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, Détection front d'onde, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, atmospheric effects
Abstract: International audience; Context. Extremely Large Telescopes have chosen the Pyramid wavefront sensor (PyWFS) over the more widely used Shack-Hartmann WaveFront Sensor (SHWFS) to perform their Single Conjugate Adaptive Optics (SCAO) mode. The PyWFS is a Fourier-filtering based sensor, which has proven to be strongly efficient for astronomical purposes. However, it shows non-linearity behaviors that lead to a reduction of its sensitivity when working around a non-null phase. This effect, called Optical Gains (OG), degrades the performance of the closed loop and prevents accurate correction of Non-Common-Path Aberrations (NCPA). Aims. We aim at computing these so-called OG with a fast and agile technique in order to control the PyWFS measurements for adaptive optics closed-loop systems. Methods. Thanks to a new theoretical description of the PyFWS, which uses a convolutional model to describe the sensor, we analytically predict the behavior of the PyWFS in closed-loop operation. This model allows us to explore the impact of residual phases on the properties of the PyFWS measurements in terms of sensitivity, and associated OG. The proposed method relies on the knowledge of the residual phase statistics and allows to automatically estimate the current OG. End-to-End numerical simulations are used to validate our predictions and test the relevance of our approach. Results. We show that an accurate estimation of the OGs is possible by only using the AO telemetry data to derive statistical information of the turbulence. The method is then fully non-invasive. We further show that by only having an estimation of the current Fried parameter r 0 and the basic system characteristics, OGs can be estimated within 10% accuracy. The proposed method applies to Pyramid WFS, but also to any Fourier-Filtering WFS suffering from OG variations.; Le contexte. Les télescopes extrêmement grands ont choisi le capteur de front d'onde Pyramid (PyWFS) plutôt que le capteur Shack-HartmannWaveFront (SHWFS) plus largement utilisé pour effectuer leur mode SCAO (Single Conjugate Adaptive Optics). Le PyWFS est un capteur basé sur un filtrage de Fourier, qui s'est avéré très efficace à des fins astronomiques. Cependant, il montre des comportements de non-linéarité qui conduisent à une réduction de sa sensibilité lors du travail autour d'une phase non nulle. Cet effet, appelé Gains optiques (OG), dégrade les performances de la boucle fermée et empêche la correction précise des aberrations non communes (NCPA). Objectifs. Nous visons à calculer ces soi-disant OG avec une technique rapide et agile afin de contrôler les mesures PyWFS pour les systèmes en boucle fermée d'optique adaptative. Méthodes. Grâce à une nouvelle description théorique du PyFWS, qui utilise un modèle convolutionnel pour décrire le capteur, nous prédisons analytiquement le comportement du PyWFS en fonctionnement en boucle fermée. Ce modèle nous permet d'explorer l'impact des phases résiduelles sur les propriétés des mesures PyFWS en termes de sensibilité et OG associées. La méthode proposée s'appuie sur la connaissance des statistiques de phase résiduelle et permet d'estimer automatiquement l'OG actuel. Des simulations numériques de bout en bout sont utilisées pour valider nos prédictions et tester la pertinence de nos approches. Résultats. Nous montrons qu'une estimation précise des OG est possible en utilisant uniquement les données de télémétrie AO pour dériver des informations statistiques de la turbulence. La méthode est alors totalement non invasive. Nous montrons en outre qu'en n'ayant qu'une estimation du paramètre de Fried r0 actuel et des caractéristiques de base du système, les OG peuvent être estimés avec une précision de 10%. La méthode proposée s'applique à Pyramid WFS, mais également à tout WFS à filtrage de Fourier subissant des variations OG.
Published: 2020

43. Imaging multiple cortical areas with high spatio-temporal resolution using innovative wide-field imaging system

Author: Pascal Weber, Jean-François Sauvage, Marc Ferrari, Audrey Bourdet, Wilfried Jahn, Emmanuel Hugot, Ivo Vanzetta, Sébastien Roux, Isabelle Racicot, Sandrine Chemla, Manon Bourbousson, Thibault Behaghel, Eduard Muslimov, Frédéric Chavane, Kevin Blaize, Institut de Neurosciences de la Timone (INT), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), CURVE-One, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, and chavane, frederic
Subjects: Heartbeat, Computer science, Brain activity and meditation, LEDs, [SDV]Life Sciences [q-bio], [SDV.NEU.NB]Life Sciences [q-bio]/Neurons and Cognition [q-bio.NC]/Neurobiology, Field of view, non-human primate, Curvature, 01 natural sciences, mesoscopic scale, 010309 optics, 03 medical and health sciences, optical imaging, 0302 clinical medicine, curved sensors, Cortex (anatomy), 0103 physical sciences, medicine, Computer vision, business.industry, [SDV] Life Sciences [q-bio], medicine.anatomical_structure, cortex, Temporal resolution, visual system, Artificial intelligence, Scale (map), Focus (optics), business, 030217 neurology & neurosurgery, Neuroscience
Abstract: International audience; Recording brain activity at the mesoscopic scale has a strong potential to unveil many new fundamental neuronal operations. Optical imaging offers a unique opportunity to measure brain activity over a large area with high spatio-temporal resolutions (20 µm x 1 ms). However, two major limitations of this imaging technique partially explain the lack of development in this field. The cortex being non-planar, the field's depth limits the region in focus to a small region close to the center of the field of view. This is particularly significant for the highly curved lissencephalic small cortex of non-human primates that are becoming popular in neuroscience experiments. The ideal technique would be a method that compensates for such curvature; it would enable imaging the whole visual system at once, from the primary to the fifth visual cortices, in small non-human primates. Additionally, the signal-to-noise ratio is strongly degraded by the dynamic evolution of the brain curvature due to physiological rhythms (heartbeat, breathing, etc.). This strongly limits the ability to work at a single-trial level and to unravel the real dynamics of neuronal processing, such as spatio-temporal waves. Here in this project, we present an interdisciplinary approach for imaging of the non-human primate cortex, using technologies from astronomical instrumentation to overcome current technological limits. This will be of interest to a wide neuroscientific audience but also will impact the clinical community interested in mapping the nervous activity at the mesoscopic scale. Our current preliminary development involves redesigning the illumination source and the optical design.
Published: 2020

44. K-Stacker: an algorithm to hack the orbital parameters of planets hidden in high-contrast imaging: First applications to VLT/SPHERE multi-epoch observations

Author: Jean-Luc Beuzit, Arthur Vigan, Markus Feldt, Kjetil Dohlen, H. Le Coroller, E. Sissa, A. L. Maire, Pierre Vernazza, A. Schneeberger, Anthony Cheetham, S. Rochat, Michael R. Meyer, Thierry Fusco, Mariangela Bonavita, D. Estevez, D. Le Mignant, François Ménard, Joany Andreina Manjarres Ramos, Matthias Samland, Mathias Nowak, Mickael Bonnefoy, J. C. Lambert, Alice Zurlo, Valentina D'Orazi, Dino Mesa, Philippe Delorme, A. Boccaletti, Hervé Beust, R. Galicher, Roxanne Ligi, Gael Chauvin, A-M. Lagrange, Markus Janson, T. Fenouillet, Raffaele Gratton, David Mouillet, L. Arnold, M. Devinat, Silvano Desidera, Maud Langlois, J. Bec-Canet, C. Desgrange, Jean-François Sauvage, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Astronomy, Stockholm University, Department of Biochemistry and Molecular Biology, Mayo Clinic, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, University of Copenhagen = Københavns Universitet (KU), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), and University of Copenhagen = Københavns Universitet (UCPH)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], planets and satellites: dynamical evolution and stability, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Context (language use), Astrophysics, instrumentation: adaptive optics, 01 natural sciences, stars: individual: HD 95086, 03 medical and health sciences, Planet, instrumentation: high angular resolution, 0103 physical sciences, Gemini Planet Imager, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 030304 developmental biology, Orbital elements, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 0303 health sciences, stars: individual: β Pictoris, Astronomy and Astrophysics, Astrometry, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], methods: data analysis, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Orbital motion, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, Astrophysics - Earth and Planetary Astrophysics
Abstract: Recent high-contrast imaging surveys, looking for planets in young, nearby systems showed evidence of a small number of giant planets at relatively large separation beyond typically 20 au where those surveys are the most sensitive. Access to smaller physical separations between 5 and 20 au is the next step for future planet imagers on 10 m telescopes and ELTs in order to bridge the gap with indirect techniques (radial velocity, transit, astrometry with Gaia). In that context, we recently proposed a new algorithm, Keplerian-Stacker, combining multiple observations acquired at different epochs and taking into account the orbital motion of a potential planet present in the images to boost the ultimate detection limit. We showed that this algorithm is able to find planets in time series of simulated images of SPHERE even when a planet remains undetected at one epoch. Here, we validate the K-Stacker algorithm performances on real SPHERE datasets, to demonstrate its resilience to instrumental speckles and the gain offered in terms of true detection. This will motivate future dedicated multi-epoch observation campaigns in high-contrast imaging to search for planets in emitted and reflected light. Results. We show that K-Stacker achieves high success rate when the SNR of the planet in the stacked image reaches 7. The improvement of the SNR ratio goes as the square root of the total exposure time. During the blind test and the redetection of HD 95086 b, and betaPic b, we highlight the ability of K-Stacker to find orbital solutions consistent with the ones derived by the state of the art MCMC orbital fitting techniques, confirming that in addition to the detection gain, K-Stacker offers the opportunity to characterize the most probable orbital solutions of the exoplanets recovered at low signal to noise., Comment: Astronomy & Astrophysics accepted, 13 Pages, 11 Figures
Published: 2020

45. The SPHERE infrared survey for exoplanets (SHINE)

Author: Kjetil Dohlen, André Müller, C. Petit, A. Pavlov, Valentina D'Orazi, Alexandre Emsenhuber, Alice Zurlo, E. Sissa, Ronald Roelfsema, Norbert Hubin, Marc Jaquet, Gabriel-Dominique Marleau, Gérard Rousset, Anthony Cheetham, H. Le Coroller, Alain Roux, S. Brown Sevilla, Enrico Giro, Faustine Cantalloube, Anne Costille, Janis Hagelberg, Jean-Luc Beuzit, Thierry Fusco, P. Gigan, Julien Charton, Markus Feldt, A. Bazzon, Ruben Asensio-Torres, C. Fontanive, Zahed Wahhaj, Anne-Lise Maire, Th. Henning, M. Carle, Marcel Carbillet, J. Ramos, Matthias Samland, Alain Origne, Raffaele Gratton, Arthur Vigan, Stéphane Udry, H. M. Schmid, Pierre Baudoz, Patrice Martinez, Markus Janson, O. Möller-Nilsson, L. Weber, Marcos Suarez, Cecile Gry, Michael Meyer, Sergio Messina, N. Engler, Emmanuel Hugot, Arnaud Sevin, A. Boccaletti, Alexander J. Bohn, P. Rabou, Julien Girard, T. Moulin, Jacopo Antichi, Beth Biller, F. Rigal, David Mouillet, C. Soenke, F. Madec, Riccardo Claudi, Silvano Desidera, M. Llored, E. Cascone, Daniela Fantinel, D. Gisler, R. Galicher, J. Baudrand, T. O. B. Schmidt, J. Pragt, Mickael Bonnefoy, D. Le Mignant, Mariangela Bonavita, Philippe Delorme, Jean-François Sauvage, Francois Wildi, Duncan Forgan, C. Mordasini, L. Gluck, Denis Perret, E. L. Rickman, Carsten Dominik, C. Lazzoni, E. Lagadec, Roxanne Ligi, Andrea Baruffolo, Lyu Abe, Gael Chauvin, A-M. Lagrange, Massimo Turatto, Pascal Puget, Philippe Feautrier, Yves Magnard, Bernardo Salasnich, Maud Langlois, V. De Caprio, D. Maurel, M. Kasper, Ken Rice, Dino Mesa, S. Rochat, C. Moutou, C. Perrot, Alain Delboulbé, P. Blanchard, François Ménard, Eric Stadler, Low Energy Astrophysics (API, FNWI), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Center for Space and Habitability (CSH), University of Bern, University of Edinburgh, Max Planck Institute for Radio Astronomy, Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Scottish Universities Physics Alliance (SUPA), Max Planck Institute for Astronomy (MPIA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Department of Biochemistry and Molecular Biology, Mayo Clinic, INAF - Osservatorio Astrofisico di Catania (OACT), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), CHU Tenon [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), CHU Pitié-Salpêtrière [AP-HP], Laboratoire des biomolécules (LBM UMR 7203), Chimie Moléculaire de Paris Centre (FR 2769), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen], European Southern Observatory (ESO), Environnements et Paléoenvironnements OCéaniques (EPOC), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Institut de Recherche pour le Développement (IRD), Centre Hospitalier Henri Duffaut (Avignon), ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), University of Michigan [Ann Arbor], University of Michigan System, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre for Exoplanet Science, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, University of Geneva [Switzerland], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Universidad Diego Portales [Santiago] (UDP), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Radboud university [Nijmegen], DAAA, ONERA, Université Paris Saclay [Meudon], Eberhard Karls Universität Tübingen, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Lagrange, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS., Laboratoire de Biomécanique et Mécanique des Chocs (LBMC UMR T9406 ), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Université Gustave Eiffel, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), CHU Tenon [APHP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université, Département Médico-Universitaire APPROCHES, Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université-Sorbonne Université (SU), Sorbonne Université-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Institut National de la Santé et de la Recherche Médicale (INSERM)-Chimie Moléculaire de Paris Centre (FR 2769), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, ARCHEORIENT - Environnements et sociétés de l'Orient ancien (Archéorient), Université Lumière - Lyon 2 (UL2)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Institut des sciences analytiques et de physico-chimie pour l'environnement et les materiaux (IPREM), Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción - University of Concepcion [Chile], Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Chimie Moléculaire de Paris Centre (FR 2769), Institut de Chimie du CNRS (INC)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), and Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: astro-ph.SR, astro-ph.GA, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, planets and satellites: formation, 10. No inequality, infrared: planetary systems, 010303 astronomy & astrophysics, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Very Large Telescope, methods: statistical, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, techniques: high angular resolution, Astronomy and Astrophysics, Planetary system, Astrophysics - Astrophysics of Galaxies, Exoplanet, Accretion (astrophysics), Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: The SHINE project is a 500-star survey performed with SPHERE on the VLT for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 MJup and semimajor axes between 5 and 300 au. We adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a MCMC tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are $23.0_{-9.7}^{+13.5}\%$, $5.8_{-2.8}^{+4.7}\%$, and $12.6_{-7.1}^{+12.9}\%$ for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1-75 MJup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of $5.7_{-2.8}^{+3.8}\%$, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies., Comment: 24 pages, 14 figures, 3 tables. Accepted for publication in A&A
Published: 2020

46. Investigating point sources in MWC 758 with SPHERE

Author: Yves Magnard, Christian Ginski, Faustine Cantalloube, Mariangela Bonavita, Gérard Rousset, Mickael Bonnefoy, Maud Langlois, C. Lazzoni, Markus Feldt, Beth Biller, A. Boccaletti, Arthur Vigan, Valentina D'Orazi, Jean-François Sauvage, Dino Mesa, François Ménard, S. B. Brown-Sevilla, Raffaele Gratton, Myriam Benisty, R. Galicher, Joany Andreina Manjarres Ramos, Silvano Desidera, C. Perrot, Gael Chauvin, A-M. Lagrange, Michael Meyer, Janis Hagelberg, Eric Pantin, Alice Zurlo, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut de sciences exactes et appliquées (ISEA), Université de la Nouvelle-Calédonie (UNC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Edinburgh, Max Planck Institute for Astronomy (MPIA), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Max Planck Institute for Radio Astronomy, Geneva Observatory, University of Geneva [Switzerland], Department of Biochemistry and Molecular Biology, Mayo Clinic, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), and Low Energy Astrophysics (API, FNWI)
Subjects: L band, Opacity, Image Processing, FOS: Physical sciences, Individual, techniques: image processing, Context (language use), Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Point (geometry), Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, planet-disk interactions, Spiral galaxy, 010308 nuclear & particles physics, protoplanetary disks, techniques: high angular resolution, Astronomy and Astrophysics, Stars, MWC 758, Techniques, Space and Planetary Science, stars: individual: MWC 758, Astrophysics::Earth and Planetary Astrophysics, High Angular Resolution, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Protoplanet, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. Spiral arms in protoplanetary disks could be shown to be the manifestation of density waves launched by protoplanets and propagating in the gaseous component of the disk. At least two point sources have been identified in the L band in the MWC 758 system as planetary mass object candidates. Aims. We used VLT/SPHERE to search for counterparts of these candidates in the H and K bands, and to characterize the morphology of the spiral arms . Methods. The data were processed with now-standard techniques in high-contrast imaging to determine the limits of detection, and to compare them to the luminosity derived from L band observations. Results. In considering the evolutionary, atmospheric, and opacity models we were not able to confirm the two former detections of point sources performed in the L band. In addition, the analysis of the spiral arms from a dynamical point of view does not support the hypothesis that these candidates comprise the origin of the spirals. Conclusions. Deeper observations and longer timescales will be required to identify the actual source of the spiral arms in MWC 758., Accepted for publication in Astronomy and Astrophysics
Published: 2021

47. Single-Mode Fiber Coupling with Adaptive Optics for Free-Space Optical Communication under Strong Scintillation

Author: A. Montmerle-Bonnefois, Bruno Fleury, Nicolas Vedrenne, Vincent Michau, Jean-Marc Conan, Serge Meimon, Jean-François Sauvage, F. Mendez, J. Montri, Cyril Petit, C. B. Lim, Philippe Perrault, DOTA, ONERA, Université Paris Saclay [Châtillon], and ONERA-Université Paris-Saclay
Subjects: Physics, [PHYS]Physics [physics], Scintillation, single-mode fiber coupling, business.industry, Phase (waves), 020206 networking & telecommunications, 02 engineering and technology, 01 natural sciences, Signal, adaptive optics, 010309 optics, Coupling (electronics), Optics, Amplitude, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, free-space optical communication, Fiber, business, Adaptive optics, ComputingMilieux_MISCELLANEOUS, Free-space optical communication
Abstract: International audience; The need for space-ground data transmission systems with high data throughput has encouraged the development of new satellite-to-ground laser links, using adaptive optics to compensate for the deleterious effects of atmospheric turbulence. On the ground segment, the use of single-mode fiber components, and thus the coupling of the propagating signal into a single-mode fiber, is strongly favored. However, the single-mode fiber coupling efficiency and the resulting data rate are strongly hampered by the turbulenceinduced phase distortions and amplitude fluctuations (called "scintillation"). The effects of scintillation in the pupil are the strongest at low elevations of Low Earth Orbit satellites-toground links and are not compensated by traditional adaptive optics, which correct only the phase of the distorted signal. In this paper, we assess the effects of AO correction on the statistical properties of single-mode fiber coupled flux based on experimental data obtained in the presence of medium and strong scintillation. We show preliminary results of coupled flux, as well as their temporal variations and probability distribution, for different adaptive optics correction levels.
Published: 2019

48. First Experimental Demonstration of Adaptive Optics Pre-Compensation for GEO Feeder Links in a Relevant Environment

Author: Bruno Fleury, Jean-François Sauvage, C. Petit, C. Voland, A. Montmerle-Bonnefois, C. B. Lim, Zoran Sodnik, Serge Meimon, J. Montri, N. Védrenne, P. Perrault, Jean-Marc Conan, F. Mendez, V. Michau, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Agence Spatiale Européenne (ESA), and European Space Agency (ESA)
Subjects: [PHYS]Physics [physics], ground station for optical feeder links, Line-of-sight, Computer science, Real-time computing, 020206 networking & telecommunications, Optical power, 02 engineering and technology, 01 natural sciences, adaptive optics, Compensation (engineering), 010309 optics, Link budget, 0103 physical sciences, Telecommunications link, 0202 electrical engineering, electronic engineering, information engineering, Adaptive optics, Throughput (business), ComputingMilieux_MISCELLANEOUS, anisoplanatism, Communication channel
Abstract: International audience; The future of very high throughput optical links between the ground and GEO satellites depends on the ability to overcome turbulence channel disruptions caused by the optical propagation through the atmosphere. Pre-compensation by adaptive optics has been identified as a game changer, as it could theoretically provide for the uplink the additional margin necessary to secure the link budget. Several experimental activities have been reported to investigate the practical increase that can be expected from AO pre-compensation, demonstrating very promising results. Due to the proximity of the line of sight from ground and the strong variability of turbulence conditions these results would benefit from a confirmation on a more representative line of sight. The line of sight between ESA's Optical Ground Station and the top of Mount Teide provides an unprecedented opportunity to provide this confirmation in a relevant environment. We report here the results of the first experimental demonstration of uplink pre-compensation performed on this line of sight in April 2019. The increase of average optical power is demonstrated and compared to expected performance. The influence of anisoplanatism is demonstrated and quantified; consequences on the future of GEO feeder links are inferred.
Published: 2019

49. High-contrast imager for complex aperture telescopes (HiCAT): 6. Two deformable mirror wavefront control (Conference Presentation)

Author: Anand Sivaramakrishnan, Iva Laginja, Ana-Maria Valenzuela, Keira Brooks, Scott D. Will, Jean-François Sauvage, Gregory R. Brady, Heather Kurtz, Peter Petrone, Roser Juanola-Parramon, Thomas Comeau, Nathan Scott, Marshall D. Perrin, Ron Shiri, Neil T. Zimmerman, Lucie Leboulleux, Julia Fowler, Rémi Soummer, Kathryn St. Laurent, Laurent Pueyo, Evelyn McChesney, Laurent M. Mugnier, Johan Mazoyer, James Noss, John G. Hagopian, Rob Gontrum, Emmanuel Hugot, Kevin Fogarty, Mamadou N'Diaye, and Marc Ferrari
Subjects: Wavefront, Computer science, Zernike polynomials, business.industry, Aperture, Astrophysics::Instrumentation and Methods for Astrophysics, Wavefront sensor, Deformable mirror, law.invention, Starlight, Telescope, symbols.namesake, Optics, law, symbols, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, Coronagraph
Abstract: The goal of the High-contrast imager for Complex Aperture Telescopes (HiCAT) testbed is to demonstrate coronagraphic starlight suppression solutions for future segmented aperture space telescopes such as the Large UV, Optical, IR telescope (LUVOIR) mission concept being studied by NASA. The testbed design has the flexibility to enable studies with increasing complexity for telescope aperture geometries starting with off-axis telescopes, then on-axis telescopes with central obstruction and support structures. The testbed implements the Apodized Pupil Lyot Coronagraph (APLC) optimized for the HiCAT aperture, which is similar to one of the possible geometries considered for LUVOIR. Wavefront can be controlled using continuous deformable mirrors, and wavefront sensing is performed using the imaging camera, or a dedicated phase retrieval camera, and also in a low-order wavefront sensing arm. We present a progress update of the testbed in particular results using two deformable mirror control to produce high-contrast dark zone, and preliminary results using the testbed’s low order Zernike wavefront sensor.
Published: 2019

50. Adaptive optics with programmable Fourier-based wavefront sensors: a spatial light modulator approach to the LAM/ONERA on-sky pyramid sensor testbed

Author: Yannick Abautret, Benoit Neichel, Kjetil Dohlen, Thierry Fusco, Charlotte Z. Bond, Kacem El-Hadi, Olivier Fauvarque, Lauren Schatz, Carlos Correia, Jean-François Sauvage, P. Janin-Potiron, Vincent Chambouleyron, Eduard Muslimov, Joseph Louis LAGRANGE (LAGRANGE), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of Coimbra, University of Coimbra [Portugal] (UC), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Image formation, Zernike polynomials, Computer science, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 01 natural sciences, adaptive optics, 010309 optics, symbols.namesake, Optics, 0103 physical sciences, pyramid wavefront sensor, Pyramid (image processing), Adaptive optics, 010303 astronomy & astrophysics, Instrumentation, ComputingMilieux_MISCELLANEOUS, Wavefront, Spatial light modulator, business.industry, Mechanical Engineering, spatial light modulator *Pierre Janin-Potiron: pierrejanin-potiron@lamfr, Fourier-based wavefront sensors, Astronomy and Astrophysics, Wavefront sensor, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Electronic, Optical and Magnetic Materials, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cardinal point, Space and Planetary Science, Control and Systems Engineering, symbols, business, optical bench
Abstract: International audience; Wavefront sensors encode phase information of an incoming wavefront into an intensity pattern that can be measured on a camera. Several kinds of wavefront sensors (WFS) are used in astronomical adaptive optics. Amongst them, Fourier-based wavefront sensors perform a filtering operation on the wavefront in the focal plane. The most well known example of a WFS of this kind is the Zernike wavefront sensor, and the pyramid wavefront sensor (PWFS) also belongs to this class. Based on this same principle, new WFSs can be proposed such as the n-faced pyramid (which ultimately becomes an axicone) or the flattened pyramid, depending on whether the image formation is incoherent or coherent. In order to test such novel concepts, the LOOPS adaptive optics testbed hosted at the Laboratoire d'Astrophysique de Marseille has been upgraded by adding a Spatial Light Modulator (SLM). This device, placed in a focal plane produces high-definition phase masks that mimic otherwise bulk optic devices. In this paper, we first present the optical design and upgrades made to the experimental setup of the LOOPS bench. Then, we focus on the generation of the phase masks with the SLM and the implications of having such a device in a focal plane. Finally, we present the first closed-loop results in either static or dynamic mode with different WFS applied on the SLM.
Published: 2019

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