使用图像恢复的Stokes成像偏振测量：基于Fabry-Pérot仪器的校准策略
Stokes imaging polarimetry using image restoration: A calibration strategy for Fabry-Pérot based instruments
摘要：
上下文：在太阳观测中，图像恢复和基于法布里-珀罗干涉仪（FPI）的仪器的组合导致特定的校准问题。FPI通常显示视场上的变化，而在图像恢复过程中，像素空间和图像空间之间的1对1关系丢失，因此使对这种变化的任何校正复杂化。目的：我们开发了一种数据简化方法，考虑到这些问题，并尽量减少由此产生的错误。方法：通过考虑望远镜的Mueller矩阵的时间变化，并使用单独的校准数据优化的波前传感在MOMFBD图像恢复过程中，并为最终的反卷积的数据，我们已经删除了大部分的校准工件从所得的数据。结果：使用这种方法来减少全斯托克斯数据从CRISP在SST，我们发现，它大大减少了仪器和图像恢复造成的空腔误差，反射率的变化，和偏振依赖性的平场的文物。结果允许有用的科学解释。使用Nicole反演代码对来自$δ$太阳黑子AR 11029的恢复数据进行反演，发现本影的盘中心侧附近有强烈的下行流（~10 km/s）。结论：结合基于FPI的仪器使用图像恢复会导致校准复杂化，并对可以实现的准确度产生固有限制。我们发现，对于CRISP，所产生的误差可以保持在偏振精度~10^-3以下。然而，旨在更高的偏振和高光谱精度的类似仪器将需要考虑这些问题。关键词：技术：图像处理，偏振，成像光谱学，太阳：表面磁性，太阳黑子，活动
英文摘要：
context: The combination of image restoration and a Fabry-Pérot interferometer (FPI) based instrument in solar observations results in specific calibration issues. FPIs generally show variations over the field-of-view, while in the image restoration process, the 1-to-1 relation between pixel space and image space is lost, thus complicating any correcting for such variations. aims: We develop a data reduction method that takes these issues into account and minimizes the resulting errors. methods: By accounting for the time variations in the telescope's Mueller matrix and using separate calibration data optimized for the wavefront sensing in the MOMFBD image restoration process and for the final deconvolution of the data, we have removed most of the calibration artifacts from the resulting data. results: Using this method to reduce full Stokes data from CRISP at the SST, we find that it drastically reduces the instrumental and image restoration artifacts resulting from cavity errors, reflectivity variations, and the polarization dependence of flatfields. The results allow for useful scientific interpretation. Inversions of restored data from the $δ$ sunspot AR11029 using the Nicole inversion code, reveal strong (~10 km/s) downflows near the disk center side of the umbra. conclusions: The use of image restoration in combination with an FPI-based instrument leads to complications in the calibrations and intrinsic limitations to the accuracy that can be achieved. We find that for CRISP, the resulting errors can be kept mostly below the polarimetric accuracy of ~10^-3. Similar instruments aiming for higher polarimetric and high spectroscopic accuracy, will, however, need to take these problems into account. keywords: Techniques: image processing, polarimetric, imaging spectroscopy, Sun: surface magnetism, sunspots, activity
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