Reconstruction methods for the phase-shifted Zernike wavefront sensor
Vincent Chambouleyron, Mahawa Cissé, Maïssa Salama, Sebastiaan Haffert, Vincent Déo, Charlotte Guthery, J. Kent Wallace, Daren Dillon, Rebecca Jensen-Clem, Phil… 展开作者
Vincent Chambouleyron, Mahawa Cissé, Maïssa Salama, Sebastiaan Haffert, Vincent Déo, Charlotte Guthery, J. Kent Wallace, Daren Dillon, Rebecca Jensen-Clem, Phil Hinz, Bruce Macintosh
The Zernike wavefront sensor (ZWFS) stands out as one of the most sensitive optical systems for measuring the phase of an incoming wavefront, reaching photon efficiencies close to the fundamental limit. This quality, combined with the fact that it can easily measure phase discontinuities, has led to its widespread adoption in various wavefront control applications, both on the ground but also for future space-based instruments. Despite its advantages, the ZWFS faces a significant challenge due to its extremely limited dynamic range, making it particularly challenging for ground-based operations. To address this limitation, one approach is to use the ZWFS after a general adaptive optics (AO) system; however, even in this scenario, the dynamic range remains a concern. This paper investigates two optical configurations of the ZWFS: the conventional setup and its phase-shifted counterpart, which generates two distinct images of the telescope pupil. We assess the performance of various reconstruction techniques for both configurations, spanning from traditional linear reconstructors to gradient-descent-based methods. The evaluation encompasses simulations and experimental tests conducted on the Santa cruz Extreme Adaptive optics Lab (SEAL) bench at UCSC. Our findings demonstrate that certain innovative reconstruction techniques introduced in this study significantly enhance the dynamic range of the ZWFS, particularly when utilizing the phase-shifted version.
The Roman Coronagraph Community Participation Program: Using the Zernike wavefront sensor for a full characterisation of the Roman Space Telescope and the Coronagraph Instrument
Aix Marseille Univ, CNRS, CNES, LAM（艾克斯马赛大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS（拉格朗日实验室，蔚蓝海岸大学，蔚蓝海岸天文台）；Jet Propulsion Laboratory, California Institute of Technology（喷气推进实验室，加州理工学院）
On-sky demonstration of a vector Zernike wavefront sensor in a cascaded adaptive optics system
ONERA（法国航空航天研究院）；Aix Marseille University, CNRS, CNES, LAM（艾克斯-马赛大学，法国国家科学研究中心，法国国家空间研究中心，拉格朗日实验室）；Aix Marseille Univ, CNRS, Pytheas, OHP, Observatoire de Haute-Provence（艾克斯-马赛大学，法国国家科学研究中心，皮泰亚斯，上普罗旺斯天文台）；Department of Physics, University of Oxford（牛津大学物理系）；W. M. Keck Observatory（W.M.凯克天文台）；Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学，蔚蓝海岸天文台，法国国家科学研究中心，拉格朗日实验室）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
Mid-order wavefront control for exoplanet imaging: preliminary characterization of the segmented deformable mirror and Zernike wavefront sensor on HiCAT
Reaching the fundamental sensitivity limit of wavefront sensing on arbitrary apertures with the Phase Induced Amplitude Apodized Zernike Wavefront Sensor (PIAA-ZWFS)
Closing the loop on-sky with a vector-Zernike wavefront sensor using a convolutional neural network as phase reconstructor
Aix Marseille Univ, CNRS, CNES, LAM（艾克斯马赛大学、法国国家科学研究中心、法国国家空间研究中心、天体物理学与行星学实验室）；DOTA, ONERA, Université Paris Saclay（ONERA航空航天研究院、巴黎萨克雷大学）；DTIS, ONERA, Université Paris Saclay（ONERA航空航天研究院、巴黎萨克雷大学）；School of Electrical Engineering, Pontificia Universidad Católica de Valparaíso（智利天主教瓦尔帕莱索大学电气工程学院）
Cascade adaptive optics with a second stage based on a Zernike wavefront sensor for exoplanet observations II. Validation in broadband light on the ESO/GHOST testbed
Université Côte d’Azur, Observatoire de la Côte d’Azur（蔚蓝海岸大学，蔚蓝海岸天文台）；Aix Marseille Université（艾克斯-马赛大学）；European Southern Observatory (ESO)（欧洲南方天文台）；University of Arizona（亚利桑那大学）
Calibration of MEMS DM actuator gains using a Zernike wavefront sensor on the HiCAT testbed and implications for Habitable Worlds Observatory operations
Space Telescope Science Institute（太空望远镜科学研究所）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学、蔚蓝海岸天文台、法国国家科学研究中心、拉格朗日实验室）
Australian Astronomical Optics, Macquarie University（澳大利亚天文光学，麦考瑞大学）；The Astrophysics and Space Technologies Research Centre, School of Mathematical and Physical Sciences, Macquarie University（麦考瑞大学数理学院天体物理与空间技术中心）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）
Millimeter-wave adaptive optics: Demonstrating closed-loop correction for lowest Zernike modes
Nagoya University（名古屋大学）；Kitami Institute of Technology（北见工业大学）；Kanazawa University（金泽大学）；Japan Women’s University（日本女子大学）；National Astronomical Observatory of Japan（日本国立天文台）；Kyoto University（京都大学）；Osaka Metropolitan University（大阪公立大学）
Analytical decomposition of Zernike and hexagonal modes over an hexagonal segmented optical aperture
ONERA The French Aerospace Laboratory（法国航空航天实验室）；Aix Marseille Université, CNRS, CNES, Laboratoire d’Astrophysique de Marseille (LAM)（艾克斯马赛大学）；Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学）
Demonstration of a photonic lantern focal-plane wavefront sensor: measurement of atmospheric wavefront error modes and low wind effect in the non-linear regime
Testing of machine learning wavefront sensing algorithms on the Tiny Observatory for Telescope Optimization (TOTO) testbed
Steward Observatory - The University of Arizona（亚利桑那大学斯图尔德天文台）；Wyant College of Optical Sciences - The University of Arizona（亚利桑那大学怀安特光学科学学院）；Department of Physics, University of California, Santa Barbara（加州大学圣塔芭芭拉分校物理系）
Demonstration of simultaneous PIAA- coronagraphy and wavefront sensing using a single metasurface-based focal-plane optic
Leiden University（莱顿大学）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；University of Arizona（亚利桑那大学）；Flatiron Institute（平顿研究所）；Subaru Telescope, National Astronomical Observatory of Japan（日本国立天文台昴星团望远镜）；National Institutes of Natural Sciences（自然科学研究机构）；Northrop Grumman Corporation（诺斯罗普·格鲁曼公司）；Draper Laboratory（德拉珀实验室）；Kirtland Air Force Base（基尔兰空军基地）；Durham University（杜伦大学）
Visible extreme adaptive optics for GMagAO-X with the triple-stage AO architecture (TSAO)
超大望远镜将需要数百个致动器穿过瞳孔，以获得可见光中的高斯特列尔。我们设想一个三级AO（TSAO）系统的GMT/GMagAO-X来实现这一点。第一级是由提供一阶校正的IR金字塔波前传感器控制的4K DM。第二级包含GMagAO-X的高阶并行DM，其具有21000个致动器，并且包含用于每个镜段的定相的干涉延迟线。该级使用Zernike波前传感器用于高阶模式，使用全息色散条纹传感器用于分段活塞控制。最后，第三阶段使用专用的3 K dm用于非共光路像差控制和通过使用焦平面波前传感和控制的日冕形波前控制。选择三级结构来创建更简单的解耦控制回路。这项工作描述了所提出的三级AO架构的性能与GMagAO-X的ExAO。
