Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.6301k&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #63.01; Bulletin of the American Astronomical Society, Vol. 24, p.1220
Astronomy and Astrophysics
Astrophysics
1
Scientific paper
In this talk we review the basics and future promise of the emerging field of interferometry at optical and infrared wavelengths. The early seventies saw the first successful deployment of independent element optical interferometers. At the current time, a number of 2-element interferometers are in routine operation. Many ambitious imaging systems have been planned or are in the process of being built. It is expected that optical/IR interferometric imaging will will have a profound effect on almost all branches of astrophysics. Consequently, it is important to understand the sensitivity and the limitations of inteferometeric imaging. The underlying theory for both optical and radio interferometers is the same, namely the van Cittert-Zernike theorem. However, there are fundamental differences in implementation. Radio interferometers operate with hetrodyned signals -- a technical convenience. Consequences include small field of view, small bandwidth and low sensitivity. In contrast, in optical interferometers, rays or beams are combined which offer large bandwidths, superior sensitivity and potentially large fields of view. Optical interferometers are fundamentally limited by photon statistics whereas radio interferometers are limited by wave noise (time bandwidth product). Atmospheric turbulence restricts the size of usable apertures, perturb path lengths and restrict integration time, all of which limit sensitivity. Imaging is possible using the technique of phase closure or self-calibration. We will review the merits and sensitivities of interferometers with different beam combinations and operating in different modes. Space based interferometers offer many advantages over ground based interferometers: high sensitivity limited only by integration time and collecting area, ultra-precise astrometry, and low background noise at IR wavelengths. The scientific gains are truly enormous. We will review a number of proposed space interferometers and also present the current status of technology readiness.
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