Abstract

Use of adaptive secondary mirrors for astronomical telescopes can have advantages over the typical adaptive optics system which use an adaptive element at a pupil relay position. The adaptive secondary replaces an optical element that already exists; therefore no additional pupil relay optics, which reduce system throughput, have to be inserted in the beam. Only one additional optic is needed between the imaging system and the primary mirror: a dichroic beamsplitter which sends the visible light to the wavefront sensor and the IR radiation to the imaging system. The ramifications of placing the adaptive element at the secondary are discussed. Also, existing telescopes can be easily retrofitted with a new secondary mirror, making installation simple.

© 1992 Optical Society of America