Abstract
The spherical aberration in the primary mirror of the Hubble Space Telescope causes more than 80% of the light from a point source to be spread into a halo of radius of 2–3 arcsec. The point spread function (PSF) is both time variant (resulting from spacecraft jitter and desorption of the secondary mirror support structure) and space variant (owing to the Cassegrain repeater optics in the Wide Field/Planetary Camera). A variety of image restoration algorithms have been utilized on HST data with some success, although optimal restorations require better modeling of the PSF and the development of efficient restoration algorithms that accommodate a space-variant PSF. The first HST servicing mission (December 1993) will deploy a corrective optics system for the Faint Object Camera and the two spectrographs and a second generation WF/PC with internal corrective optics. As simulations demonstrate, however, the restoration algorithms developed now for aberrated images will be very useful for removing the remaining diffraction features and optimizing dynamic range in post-servicing mission data.
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Hanisch, R.J., White, R.L. (1994). HST Image Restoration: Current Capabilities and Future Prospects. In: Robertson, J.G., Tango, W.J. (eds) Very High Angular Resolution Imaging. International Astronomical Union / Union Astronomique Internationale, vol 158. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0880-5_7
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DOI: https://doi.org/10.1007/978-94-011-0880-5_7
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