Abstract

In remote sensing and astronomy, images are often reconstructed from data obtained by fixed or scanning detector arrays superimposed on the image field [1]. Since detectors are typically much larger than the blur spot of the imaging optics, a naive reconstruction of the image from the detector data would produce an image of lower resolution than that furnished by the imaging optics. The reduction of detector size to match the blur spot of the imaging optics may not be technically feasible, and even if it were, the associated signal-to-noise ratio of the detector output might be too low to be useful.

© 1989 Optical Society of America