发表机构
ONERA; Aix Marseille University, CNRS, CNES, LAM; Aix Marseille Univ, CNRS, Pytheas, OHP, Observatoire de Haute-Provence; Department of Physics, University of Oxford; W. M. Keck Observatory; Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange; Jet Propulsion Laboratory, California Institute of Technology（法国航空航天研究院; 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; 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; 牛津大学物理系; W.M.凯克天文台; 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; 加州理工学院喷气推进实验室）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究在PAPYRUS平台搭建含v-ZWFS的第二级AO系统，在轨验证其闭环运行能力，使斯特列尔比提升16个百分点，为未来级联极端AO系统应用提供支撑。
AI 中文摘要
为直接成像和表征类地系外行星，未来高对比度仪器将需要工作在越来越高环路频率的自适应光学系统，以减少时间误差。提高环路频率会降低每个波前传感器帧的信噪比，因此高灵敏度波前传感器如泽尼克波前传感器（ZWFS）成为有吸引力的候选。然而，经典ZWFS的有限动态范围使其在轨运行具有挑战性。为此，我们研究ZWFS是否可作为在轨级联自适应光学系统的第二级传感器。我们在上普罗旺斯天文台的PAPYRUS平台上添加了名为OZIRIIS的第二级AO系统，该系统结合了矢量泽尼克波前传感器（v-ZWFS）与97致动器变形镜，工作在基于金字塔的第一级AO系统下游，频率为400Hz。实时控制依赖单一ZWFS信号，而完整的v-ZWFS则事后用于非线性重建和遥测分析。第二级校正使测得的斯特列尔比提高了多达16个百分点。利用完整v-ZWFS重建残差的遥测分析显示，低斯特列尔比时存在影响ZWFS的光学增益效应。在轨测量与数值模拟的良好一致性进一步支持基于合成参考信号和相互作用矩阵的校准策略。这些结果证明泽尼克波前传感可在轨闭环运行，并支持其在未来级联极端自适应光学系统中的应用。
英文摘要
To directly image and characterise Earth-like exoplanets, future high-contrast instruments will require adaptive-optics systems operating at increasingly high loop frequencies to reduce temporal errors. Increasing the loop frequency reduces the signal-to-noise ratio per wavefront-sensor frame, making highly sensitive wavefront sensors, such as the Zernike wavefront sensor (ZWFS), attractive candidates. However, the limited dynamic range of the classical ZWFS makes on-sky operation challenging. We therefore investigate whether a ZWFS can be used as a second-stage sensor in an on-sky cascaded adaptive-optics system. To this end, we added a second AO stage, called OZIRIIS, to the PAPYRUS platform at the Observatoire de Haute-Provence. OZIRIIS combines a vector Zernike wavefront sensor (v-ZWFS) with a 97-actuator deformable mirror operating at 400 Hz downstream of the pyramid-based first AO stage. Real-time control relied on a single ZWFS signal, while the full v-ZWFS was used a posteriori for non-linear reconstruction and telemetry analysis. The second-stage correction increased the measured Strehl ratio by up to 16 percentage points. Analysis of the telemetry using the full v-ZWFS to reconstruct residuals revealed optical-gain effects affecting the ZWFS at low Strehl ratio. The good agreement between on-sky measurements and numerical simulations further supports the calibration strategy based on synthetic reference signals and interaction matrices. These results demonstrate that Zernike wavefront sensing can be operated in closed loop on sky and support its use in future cascaded extreme adaptive-optics systems.
Comments11 pages, 11 figures. Accepted for publication in Astronomy & Astrophysics (A&A)
DOI：10.1051/0004-6361/202661472
