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Limitations to Optical/IR Interferometry from the Ground and Space

Published online by Cambridge University Press:  19 July 2016

M. M. Colavita*
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91101, USA

Abstract

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The primary limitation to ground-based optical/IR interferometry is the turbulent atmosphere, which limits sensitivity by restricting the coherence volume, limits imaging accuracy by corrupting the fringe phase, and limits astrometric accuracy by corrupting the angle of arrival. Various advanced techniques can be used to circumvent these limits to some extent. Sensitivity can be increased with adaptive optics and laser guide stars, which should eventually be able to phase the individual apertures of an interferometer down to some cutoff wavelength, limited by tilt sensing. However, the sky coverage for cophasing the interferometer on an arbitrary object will remain limited at short wavelengths. For imaging, closure-phase techniques, well established in radio interferometry, will be used in next-generation instruments. However, for maximum sensitivity on extended objects, redundant arrays will be needed to cophase the interferometer. For astrometry, the limits to wide-field astrometry set by the atmosphere can be reduced somewhat with two-color techniques, but otherwise do not seem reducible by the techniques now being discussed. However, over narrow fields, the astrometric performance of an interferometer can be quite good. In space, without the corruptions of the atmosphere, the fundamental limitation is photon noise. However, technical issues such as metrology accuracy and practical issues such as maximum affordable baseline length will also limit performance.

Type
Future Prospects
Copyright
Copyright © Kluwer 1994 

References

Shao, M. and Colavita, M. M. Long-baseline optical and infrared stellar interferometry. Annu. Rev. Astron. Astrophys., 30:457498, 1992.CrossRefGoogle Scholar
Fugate, R. Q., Fried, D. L., Ameer, G. A. et al. Measurement of atmospheric wavefront distortion using scattered light from a laser guide-star. Nature, 353:144146, 1991.Google Scholar
Primmerman, C. A., Murphy, D. V., Page, D. A., et al. Compensation of atmospheric optical distortion using a synthetic beacon. Nature, 353:141143, 1991.CrossRefGoogle Scholar
Rigaut, F. and Gendron, E. Laser guide star in adaptive optics -the tilt determination problem. Astron. Astrophys., 261:677, 1992.Google Scholar
Roddier, F. Passive versus active methods in optical interferometry. In High-Resolution Imaging by Interferometry, volume 29, Conf. and Workshop Proc., pages 565574. ESO, 1988.Google Scholar
Shao, M., Colavita, M. M., Hines, B. E., et al. Wide angle astrometry with the Mark III stellar interferometer. Astron. J., 100:17011711, 1990.CrossRefGoogle Scholar
Shao, M. and Colavita, M. M. Potential of long-baseline infrared interferometry for narrow-angle astrometry. Astron. Astrophys., 262:353358, 1992.Google Scholar