High angular resolution astronomical techniques - Speckle interferometry and related methods

Details High angular resolution astronomical techniques - Speckle interferometry and related methods High angular resolution astronomical techniques - Speckle interferometry and related methods

Jan 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980spie..243...66w&link_type=abstract

In: Applications of speckle phenomena; Proceedings of the Seminar, San Diego, CA, July 29, 30, 1980. (A81-39439 18-35) Bellingha

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Applications

1

Angular Resolution, Atmospheric Turbulence, Binary Stars, Image Reconstruction, Interferometry, Speckle Patterns, Astrometry, Background Noise, Correlation, High Resolution, Image Processing, Power Spectra, Statistical Analysis, Stellar Magnitude

Scientific paper

A review of speckle interferometry techniques and hardware for recovering image information degraded by turbulence (which reduces angular resolution to about 1 arcsec) in the earth's atmosphere is presented. Speckle interferometry, which relies on post processing of short exposure images, provides two orders of magnitude increase in angular resolution for studying object sizes and binary star orbits. Lynds et al. (1976) showed that images of bright stars were directly obtainable from speckle photos. For more general image reconstruction, the power spectrum used to determine angular sizes must be supplemented with Fourier phases. Knox and Thompson (1974) developed statistical techniques to get the phase from speckle photos directly; however, the techniques are highly noise sensitive and limited to bright objects like the sun. A method developed by Fienup (1978) was applied to derive phases for faint astronomical targets. The method is insensitive to noise and shows that actual diffraction-limited images can be reconstructed for objects fainter than +15 magnitudes.

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