The point spread function of the soft X-ray telescope aboard YOHKOH

Details The point spread function of the soft X-ray telescope aboard YOHKOH The point spread function of the soft X-ray telescope aboard YOHKOH

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995soph..157..141m&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 157, no. 1-2, p. 141-168

Physics

35

Fitting, Image Processing, Point Spread Functions, X Ray Imagery, X Ray Telescopes, Charge Coupled Devices, Fourier Transformation, Goodness Of Fit, Least Squares Method

Scientific paper

The point spread function of the SXT telescope aboard Yohkoh has been measured in flight configuration in three different X-ray lines at White Sands Missile Range. We have fitted these data with an elliptical generalization of the Moffat function. Our fitting method consists of chi squared minimization in Fourier space, especially designed for matching of sharply peaked functions. We find excellent fits with a reduced chi squared of order unity or less for single exposure point spread functions over most of the CCD. Near the edges of the CCD the fits are less accurate due to vignetting. From fitting results with summation of multiple exposures we find a systematic error in the fitting function of the order of 3% near the peak of the point spread function, which is close to the photon noise for typical SXT images in orbit. We find that the full width to half maximum and fitting parameters vary significantly with CCD location. However, we also find that point spread functions measured at the same location are consistent to one another within the limit determined by photon noise. A 'best' analytical fit to the PSF as function of position on the CCD is derived for use in SXT image enhancemnent routines. As an aside result we have found that SXT can determine the location of point sources to about a quarter of a 2.54 arc sec pixel.

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