用简约点扩散函数模型对大气和仪器缺陷的联合估计.用世界上最先进的自适应光学辅助仪器进行空中确认
Joint estimation of atmospheric and instrumental defects using a parsimonious point spread function model.On-sky validation using state of the art worldwide adaptive-optics assisted instruments
摘要：
由于光学点扩散函数（PSF）的复杂形状和空间变化，其建模对于自适应光学（AO）辅助观测具有特殊的挑战性。我们的目标是（i）通过与大量成像PSF样本的比较，详尽地证明最近分析模型的准确性，（ii）评估模型最佳的条件，以及（iii）释放该框架的强度，以实现联合估计大气参数、AO性能和静态像差。我们收集了从七个AO系统中获得的4812个天空PSF，并使用相同的拟合算法在各种AO PSF上测试模型，并从模型输出中诊断AO性能。最后，我们强调了这个框架如何使表征的所谓的低风效应的SPHERE仪器和活塞同相误差的凯克II望远镜。在4812个PSF上，该模型在Strehl比（SR）和半高全宽（FWHM）上的误差均达到4%。我们特别说明，Fried参数，这是一个模型参数的估计，是一致的，与已知的看到的统计，并遵循预期的趋势，波长使用MUSE仪器（$λ^{6/5}$）和字段（无变化）从GSAOI图像的标准偏差为0.4厘米。最后，我们表明，我们可以检索的差分活塞，提示和倾斜模式的LWE介绍，比较ZELDA测量，以及段活塞错误的凯克II望远镜，特别是楼梯模式，已经从以前的研究中发现的组合。该模型在4%的误差水平下匹配所有类型的AO PSF，并可用于AO诊断、后处理和波前传感目的。
英文摘要：
Modeling the optical point spread function (PSF) is particularly challenging for adaptive optics (AO)-assisted observations owing to the its complex shape and spatial variations. We aim to (i) exhaustively demonstrate the accuracy of a recent analytical model from comparison with a large sample of imaged PSFs, (ii) assess the conditions for which the model is optimal, and (iii) unleash the strength of this framework to enable the joint estimation of atmospheric parameters, AO performance and static aberrations. We gathered 4812 on-sky PSFs obtained from seven AO systems and used the same fitting algorithm to test the model on various AO PSFs and diagnose AO performance from the model outputs. Finally, we highlight how this framework enables the characterization of the so-called low wind effect on the SPHERE instrument and piston cophasing errors on the Keck II telescope. Over 4812 PSFs, the model reaches down to 4% of error on both the Strehl-ratio (SR) and full width at half maximum (FWHM). We particularly illustrate that the estimation of the Fried parameter, which is one of the model parameters, is consistent with known seeing statistics and follows expected trends in wavelength using the MUSE instrument ($λ^{6/5}$) and field (no variations) from GSAOI images with a standard deviation of 0.4cm. Finally, we show that we can retrieve a combination of differential piston, tip, and tilt modes introduced by the LWE that compares to ZELDA measurements, as well as segment piston errors from the Keck II telescope and particularly the stair mode that has already been revealed from previous studies. This model matches all types of AO PSFs at the level of 4% error and can be used for AO diagnosis, post-processing, and wavefront sensing purposes.
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