ADAPTIVE OPTICS FOR ASTRONOMY - THEORETICAL PERFORMANCE AND LIMITATIONS

We investigate the theoretical performance of adaptive optics correcti on for imaging in astronomy. Image improvements are calculated as a fu nction of the fundamental limitations imposed by anisoplanatic effects , and photon and detector noise in wavefront sensing. In contrast to p revious studies, which have concentrated mainly on predicting Strehl r atio improvements, we calculate the adaptively corrected point-spread function explicitly. The shape of the point-spread function, and encir cled energy widths, is crucial in astronomical applications such as ph otometry and spectroscopy. The analysis therefore allows a detailed as sessment of the potential benefits of adaptive optics for astronomical applications, and provides an important tool for system design.