The importance of point-spread function corrections in solar physics | Stefan Hofmeister
Leibniz Institute for Astrophysics Potsdam (AIP), Germany
Natural Sciences (Astrophysics and Astrononmy)
Point spread functions describe diffraction and scattering in imaging instruments and can be used to correct the images for the scattered light. However, mostly, the scattered light correction is not used in the solar physics community, on the one hand since many scientists are not aware of its importance, on the other hand since it can be computationaly extensive. In this talk, I will present (1) new revised point spread functions for AIA that correct for long-distance scattered light over the detector, (2) what solar features and data products are affected the most by instrumental scattered light, (3) the error involved when the scattered-light correction is neglected, (4) and a new point spread function deconvolution method. Read more at https://espos.stream/2023/05/25/Hofmeister/.
Link to the European Solar Physics Online Seminars (ESPOS) webpage:
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