Achieving high resolution in earth-based optical astronomy

Details Achieving high resolution in earth-based optical astronomy Achieving high resolution in earth-based optical astronomy

Dec 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979svphu.129..645t&link_type=abstract

(Uspekhi Fizicheskikh Nauk, vol. 129, Dec. 1979, p. 645-670.) Soviet Physics - Uspekhi, vol. 22, Dec. 1979, p. 960-974. Transla

Physics

Adaptive Filters, Astronomical Observatories, High Resolution, Michelson Interferometers, Speckle Patterns, Telescopes, Astronomical Photography, Optical Equipment, Sensitivity

Scientific paper

The resolution of ordinary astrophotographs obtained with long exposure times is the same for all objects brighter than the limit and is determined only by the atmospheric turbulence generated at existing observatories by orographic atmospheric circulation disturbances. Nonclassical, interference methods deliver much better (by factors up to 1000) resolution at the cost of very insignificant (factors up to 1000-10,000) deterioration of the ability to register faint objects. The Michelson interferometer at its modern technical level and speckle interferometry are most promising among these methods. Their sensitivity limits are determined by the quantum nature of light and depend strongly on long-exposure image quality. The intensity interferometer gives even better (now down to 0.001 arcsec) resolution, but its low sensitivity permits the use of this method only for bright stars. Adaptive optics does not appear to be widely useful in the astronomy of faint objects. A generalized relation is given for sensitivity as a function of resolution in the various techniques for resolution improvement, and prospects for their future development are discussed.

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