Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987esasp.273...69w&link_type=abstract
In ESA, ESA Workshop on Optical Interferometry in Space p 69-72 (SEE N88-10613 01-74)
Astronomy and Astrophysics
Astronomy
1
Holographic Interferometry, Spaceborne Astronomy, Speckle Patterns, Image Reconstruction, Signal To Noise Ratios, Space Erectable Structures, Spacecraft Configurations, Stellar Magnitude
Scientific paper
The construction of a large multimirror interferometer in space is proposed. Resolution of 0.001 arcsec at 100 nm is feasible with a 20 m baseline. A shuttle launched 14 m linear array, a 2 dimensional, deployable 20 m array, and arrays of 6 to 20 free-flying telescopes with baselines up to 40 km and resolution of 0.000001 arcsec at 200 nm are possible. At short UV wavelengths a multimirror interferometer will produce speckle interferograms caused by misalignment of the interferometer. From the speckle interferograms true images can be reconstructed by the phase-closure method (if the exit pupil is a nonredundant array) or by speckle masking (for general pupils). In the case of bright objects the phase-closure method yields higher signal-to-noise ratio than speckle masking. In the case of faint objects speckle masking yields higher signal-to-noise ratio than the phase-closure method. The limiting magnitude of optical long-baseline interferometry in space is 24 or fainter.
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