MMT M-band speckles computed from AO WFS vs actual Clio2 images.
Автор: Johanan Codona
Загружено: 2011-03-27
Просмотров: 513
Описание: The adaptive optics (AO) Shack-Hartmann wavefront sensor (WFS) records starlight wavefront residuals even if they cannot be corrected. The WFS uses the visible portion of the starlight to estimate the atmospherically-distorted wavefront, while infrared starlight is passed on to the science camera. Since the science light passes through different optics than the WFS light, different "non-common-path" aberrations can and do occur. This is part of an experiment to use the AO measurements to analyze and correct errors in the science camera light path. The images on the left are completely synthetic, computed from the wavefront sensor and a Fourier optics model of the MMT telescope. The image on the right is from the Clio mid-IR science camera. The real frame rate is 30 fps. The MMT AO system was being tested in new operating modes while this data was taken. This does not represent its best performance. However, since we are interested in the focal plane speckles for diagnostic purposes, this dataset is perfect! This is part of our NSF-funded Phase-Sorting Interferometry (PSI) work at the University of Arizona.
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