PSF Correction for AIA Using Lunar Limb Data
Abstract
PSF correction is important for myriad inferences that can be made from EUV imagery, including heating distribution and impulsivity; DEM; and wave amplitude measurements. Using lunar limb and solar flare data, we have prepared model PSF functions to describe the scattering performance of the six EUV channels of AIA. We have not attempted to model the core of the PSF (focus), only its wings (stray light) of each channel. We find that, typically, about half of the scattered light is in the diffuse component of the PSF model, although there is significant variation across the channels. The diffraction component of the PSF was determined by direct inspection of the diffraction pattern from flaring images, with some a priori knowledge of the physics and nature of the diffraction grid (following the methods of Gburek on TRACE and more recently, Cheung on AIA); and the diffuse component was determined by iteratively fitting imaging performance around the lunar limb in eclipse images, with the assumption that the Moon is dark in the EUV. We present the PSFs and summary data, along with a preliminary comparision with the diffraction-only models developed at SAO, and describe where to get both the quantitative PSF models and their inverses (for direct deconvolution) in FITS format.
- Publication:
-
SDO-4: Dynamics and Energetics of the Coupled Solar Atmosphere. The Synergy Between State-of-the-Art Observations and Numerical Simulations
- Pub Date:
- March 2012
- Bibcode:
- 2012decs.confE.121D
- Keywords:
-
- SDO;
- SDO-4;
- SDO 4;
- SDO Workshop;
- SDO-4/IRIS/Hinode Workshop;
- Solar Dynamic Observatory