The VLT interferometer. IV - The utility of partial adaptive optics

Details The VLT interferometer. IV - The utility of partial adaptive optics The VLT interferometer. IV - The utility of partial adaptive optics

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990spie.1236..154b&link_type=abstract

IN: Advanced technology optical telescopes IV; Proceedings of the Meeting, Tucson, AZ, Feb. 12-16, 1990. Part 1 (A91-23201 08-89

Physics

Optics

4

Adaptive Optics, Infrared Radiation, Very Large Array (Vla), Very Long Base Interferometry, Visible Spectrum, Imaging Techniques, Point Spread Functions, Spatial Filtering, Speckle Interferometry, Systems Engineering, Wave Fronts

Scientific paper

The application of full adaptive optics to astronomical telescopes in the foreseeable future is likely to be limited to infrared wavelengths greater than 1 micron both because of the limited number of bright enough wavefront sensing objects at visible wavelengths and because of the complexity and expense of making an adaptive optics system for large telescopes with the large number of elements required at visible wavelengths. Adaptive optics designed for infrared wavelengths do, however, improve the image quality at wavelengths shorter than the design wavelength, thus improving the sensitivity of interferometric imaging at those wavelengths.

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