Integrated photonic-based coronagraphic systems for future space telescopes

The detection and characterization of Earth-like exoplanets around Sun-like stars is a primary science motivation for the Habitable Worlds Observatory. However, the current best technology is not yet advanced enough to reach the 10^-10 contrasts at close angular separations and at the same time remain insensitive to low-order aberrations, as would be required to achieve high-contrast imaging of exo-Earths. Photonic technologies could fill this gap, potentially doubling exo-Earth yield. We review current work on photonic coronagraphs and investigate the potential of hybridized designs which combine both classical coronagraph designs and photonic technologies into a single optical system. We present two possible systems. First, a hybrid solution which splits the field of view spatially such that the photonics handle light within the inner working angle and a conventional coronagraph that suppresses starlight outside it. Second, a hybrid solution where the conventional coronagraph and photonics operate in series, complementing each other and thereby loosening requirements on each subsystem. As photonic technologies continue to advance, a hybrid or fully photonic coronagraph holds great potential for future exoplanet imaging from space.Comment: Conference Proceedings of SPIE: Techniques and Instrumentation for Detection of Exoplanets XI, vol. 12680 (2023

Visible extreme adaptive optics on extremely large telescopes: Towards detecting oxygen in Proxima Centauri b and analogs

Looking to the future of exo-Earth imaging from the ground, core technology developments are required in visible extreme adaptive optics (ExAO) to enable the observation of atmospheric features such as oxygen on rocky planets in visible light. UNDERGROUND (Ultra-fast AO techNology Determination for Exoplanet imageRs from the GROUND), a collaboration built in Feb. 2023 at the Optimal Exoplanet Imagers Lorentz Workshop, aims to (1) motivate oxygen detection in Proxima Centauri b and analogs as an informative science case for high-contrast imaging and direct spectroscopy, (2) overview the state of the field with respect to visible exoplanet imagers, and (3) set the instrumental requirements to achieve this goal and identify what key technologies require further development.Comment: SPIE Proceeding: 2023 / 12680-6

Post-coronagraphic wavefront sensing and control for exoplanet imaging

L’imagerie d’exoplanètes est limitée par deux obstacles intrinsèques : le faible écart angulaire entre planète et étoile, et le très faible flux lumineux en provenance de la planète par rapport à la lumière de l’étoile. Le premier obstacle est surmonté par l’utilisation de très grands télescopes, de la classe des dix mètres de diamètre, et éventuellement depuis le sol de systèmes d’optique adaptative, qui permettent d’atteindre de hautes résolutions angulaires. Le deuxième obstacle est surmonté par l’utilisation de coronographes. Les coronographes sont des instruments conçus pour filtrer la lumière de l’étoile tout en laissant passer la lumière de l’environnement circumstellaire. Cependant, toute aberration optique en amont du coronographe engendre des fuites de lumière stellaire à travers le coronographe. Ces fuites se traduisent par un fouillis de tavelures dans les images scientifiques, tavelures qui cachent d’éventuelles planètes. Il est donc nécessaire de mesurer et de corriger les aberrations quasi-statiques à l’origine des tavelures. Cette thèse présente des contributions théoriques, numériques et expérimentales à la mesure et à la correction des aberrations des imageurs coronographiques. La première partie décrit le contexte et présente la méthode de la diversité de phase coronographique, un formalisme qui considère l’analyse de surface d’onde post-coronographique comme un problème inverse posé dans un cadre bayésien. La deuxième partie concerne l’imagerie depuis le sol. Elle présente tout d’abord une expression analytique permettant de modéliser l’imagerie coronographique en présence de turbulence, puis l’extension de la méthode de diversité de phase coronographique à la mesure depuis les télescopes au sol donc en présence de turbulence résiduelle, et enfin une validation en laboratoire de cette méthode étendue. La troisième partie est consacrée aux futurs imageurs spatiaux à très hauts contrastes pour lesquels il faut corriger non pas seulement la phase mais tout le champ complexe. Elle présente la validation en laboratoire de la mesure d’un champ complexe d’aberrations par diversité de phase coronographique, ainsi que des premiers résultats d’extinction de la lumière en plan focal par une méthode non linéaire, le non-linear dark hole.Exoplanet imaging has two intrinsic limitations, namely the small angular separation between the star and the planet, and the very low light flux from the planet compared to the starlight. The first limitation is overcome by using very large telescopes of the ten-metre diameter class, and, for ground-based telescopes, adaptive optics systems, which allow high angular resolution imaging. The second limitation is overcome by using a coronagraph. Coronagraphs are optical devices which filter the starlight while granting passage to the light coming from the stellar environment. However, any optical aberration upstream of the coronagraph causes some of the starlight to leak through the coronagraph. This unfiltered starlight in turn causes speckles in the scientific images, and the light of the planets that could be there is lost among the speckles. Consequently, measurement and correction of the quasi-static aberration which generate the speckles are necessary for the exoplanet imagers to achieve their full potential. This thesis introduces theoretical, numerical, and experimental contributions to the topic of measurement and correction of the aberrations in coronagraphic imagers. The first part describes the context and introduces coronagraphic phase diversity, which is a Bayesian inverse problem formalism for post-coronagraphic wave-front sensing. The second part is focused on ground-based imaging. It introduces an analytic expression for coronagraphic imaging through turbulence, the extension of coronagraphic phase diversity to on-sky measurement through residual turbulence, and a laboratory validation of the extended method. The third part is concerned with future high-contrast space-based imagers, which will require not only phase correction, but a full complex wave-front correction. It presents the laboratory validation of coronagraphic phase diversity as a post-coronagraphic complex wave-front sensor, and first results of active contrast enhancement in the focal plane through thecreation of a non-linear dark hole

Analyse et correction de surface d’onde post-coronographique pour l’imagerie d’exoplanètes

Exoplanet imaging has two intrinsic limitations, namely the small angular separation between the star and the planet, and the very low light flux from the planet compared to the starlight. The first limitation is overcome by using very large telescopes of the ten-metre diameter class, and, for ground-based telescopes, adaptive optics systems, which allow high angular resolution imaging. The second limitation is overcome by using a coronagraph. Coronagraphs are optical devices which filter the starlight while granting passage to the light coming from the stellar environment. However, any optical aberration upstream of the coronagraph causes some of the starlight to leak through the coronagraph. This unfiltered starlight in turn causes speckles in the scientific images, and the light of the planets that could be there is lost among the speckles. Consequently, measurement and correction of the quasi-static aberration which generate the speckles are necessary for the exoplanet imagers to achieve their full potential. This thesis introduces theoretical, numerical, and experimental contributions to the topic of measurement and correction of the aberrations in coronagraphic imagers. The first part describes the context and introduces coronagraphic phase diversity, which is a Bayesian inverse problem formalism for post-coronagraphic wave-front sensing. The second part is focused on ground-based imaging. It introduces an analytic expression for coronagraphic imaging through turbulence, the extension of coronagraphic phase diversity to on-sky measurement through residual turbulence, and a laboratory validation of the extended method. The third part is concerned with future high-contrast space-based imagers, which will require not only phase correction, but a full complex wave-front correction. It presents the laboratory validation of coronagraphic phase diversity as a post-coronagraphic complex wave-front sensor, and first results of active contrast enhancement in the focal plane through thecreation of a non-linear dark hole.L’imagerie d’exoplanètes est limitée par deux obstacles intrinsèques : le faible écart angulaire entre planète et étoile, et le très faible flux lumineux en provenance de la planète par rapport à la lumière de l’étoile. Le premier obstacle est surmonté par l’utilisation de très grands télescopes, de la classe des dix mètres de diamètre, et éventuellement depuis le sol de systèmes d’optique adaptative, qui permettent d’atteindre de hautes résolutions angulaires. Le deuxième obstacle est surmonté par l’utilisation de coronographes. Les coronographes sont des instruments conçus pour filtrer la lumière de l’étoile tout en laissant passer la lumière de l’environnement circumstellaire. Cependant, toute aberration optique en amont du coronographe engendre des fuites de lumière stellaire à travers le coronographe. Ces fuites se traduisent par un fouillis de tavelures dans les images scientifiques, tavelures qui cachent d’éventuelles planètes. Il est donc nécessaire de mesurer et de corriger les aberrations quasi-statiques à l’origine des tavelures. Cette thèse présente des contributions théoriques, numériques et expérimentales à la mesure et à la correction des aberrations des imageurs coronographiques. La première partie décrit le contexte et présente la méthode de la diversité de phase coronographique, un formalisme qui considère l’analyse de surface d’onde post-coronographique comme un problème inverse posé dans un cadre bayésien. La deuxième partie concerne l’imagerie depuis le sol. Elle présente tout d’abord une expression analytique permettant de modéliser l’imagerie coronographique en présence de turbulence, puis l’extension de la méthode de diversité de phase coronographique à la mesure depuis les télescopes au sol donc en présence de turbulence résiduelle, et enfin une validation en laboratoire de cette méthode étendue. La troisième partie est consacrée aux futurs imageurs spatiaux à très hauts contrastes pour lesquels il faut corriger non pas seulement la phase mais tout le champ complexe. Elle présente la validation en laboratoire de la mesure d’un champ complexe d’aberrations par diversité de phase coronographique, ainsi que des premiers résultats d’extinction de la lumière en plan focal par une méthode non linéaire, le non-linear dark hole

Shadow Imaging of Geostationary Satellites: silhouette reconstruction from accurate polychromatic modelling of diffraction and atmospheric disturbances

International audienceShadow imaging is a very promising technique for imaging the silhouette of geostationary satellites at submetric resolutions from the ground. The method is based on the numerical inversion of the shadow cast by the satellite when it occults a star. We have built an inversion algorithm based both on a fine physical modelling of light propagation, and that makes full use of the polychromatic flux of the star. We conducted several simulations to show a few realistic working examples, giving special attention to shadow sampling. We also proved that the chromatic inversion allows for a considerable improvement in the reconstruction

An analytic expression for coronagraphic imaging through turbulence. Application to on-sky coronagraphic phase diversity

International audienceThe ultimate performance of coronagraphic high-contrast exoplanet imaging systems such as SPHERE or GPI is limited by quasi-static aberrations. These aberrations produce speckles that can be mistaken for planets in the image. In order to design instruments, correct quasi-static aberrations or analyse data, the expression of the point spread function of a coronagraphic instrument in the presence of residual turbulence is most useful. Here, we derive an analytic expression for this point spread function that is an extension to coronagraphic imaging of Roddier's expression for imaging through turbulence. We give a physical interpretation of its structure, we validate it by numerical simulations and we show that it is computationally efficient. Finally, we incorporate this imaging model into a coronagraphic phase diversity method (COFFEE) and validate by simulations that it allows wave-front reconstruction in the presence of residual turbulence. The preliminary results, which give a sub-nanometric precision in the case of a SPHERE-like system, strongly suggest that quasi-static aberrations could be calibrated during observations by this method

A simple ionospheric correction method for radar-based space surveillance systems, with performance assessment on GRAVES data

Ionospheric effects degrade the quality of radar data, which are critical for the precision of the satellite ephemeris produced by space surveillance systems; this degradation is especially noticeable for radars such as GRAVES that operate in the very high frequency range. This article presents a simple and effective method to correct for ionospheric effects, with an evaluation on data obtained with GRAVES, the French space surveillance radar. This method relies on GPS data, and our evaluation relies on GRAVES and DORIS data. We found that the gain in terms of evaluated radial velocity can be as high as 1.76$\kappa$, where $\kappa$ is the typical root mean square of the noise on radial velocity measurements for GRAVES (excluding ionospheric effects): the error decreases from 2.60$\kappa$ to 0.83$\kappa$ for daytime satellite overhead passes. Our conclusion is that, while this method is very simple to implement, it has proven to be a good correction for ionospheric effects in practice.Comment: Accepted for publication in Advances in Space Research. 6 pages, 4 figure

Correction de front d'onde plan focal par apprentissage par renforcement sans modèle

International audienceOptical aberrations prevent telescopes from reaching their theoretical diffraction limit. Once estimated, these aberrations can be compensated for using deformable mirrors in a closed loop. Focal plane wavefront sensing enables the estimation of the aberrations on the complete optical path, directly from the images taken by the scientific sensor. However, current focal plane wavefront sensing methods rely on physical models whose inaccuracies may limit the overall performance of the correction. The aim of this study is to develop a data-driven method using model-free reinforcement learning to automatically perform the estimation and correction of the aberrations, using only phase diversity images acquired around the focal plane as inputs. We formulate the correction problem within the framework of reinforcement learning and train an agent on simulated data. We show that the method is able to reliably learn an efficient control strategy for various realistic conditions. Our method also demonstrates robustness to a wide range of noise levels