High resolution astronomical imaging by post-detection image processing

Advances in image-reconstruction techniques and computation capability have made it practical to use post-detection processing to overcome the resolution limits imposed on conventional astronomical observations by turbulence in the atmosphere. Techniques based on second and third-order spectra have proved to be very successful. The astronomical application requires special attention to the calibration of the measured atmospheric transfer function, the removal of photon-noise biases and the effects of finite detector size. A new area of application is the enhancement of images partially compensated by adaptive optics