24 July 1998 Aperture synthesis imaging with the Keck Interferometer
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JPL and CARA are building a multi-element, IR interferometer for NASA to be situated at the twin Keck Observatories on Mauna Kea, Hawaii. Initially, the 10-m diameter Keck telescopes will be augmented with four fixed-location 2-m class outrigger telescopes resulting in 15 non-redundant baselines, the longest being approximately equals 110 m or nearly 5 X 107 ((lambda) /2.2micrometers )-1 wavelengths. Fast adaptive optics and tip-tilt corrections will be used to phase up the Keck and outrigger apertures, respectively. The entire array will be co-phased by observing a relatively bright target on the photon rich Keck-Keck (K-K) and Keck- outrigger (K-O) baselines. When fully phased, the projected fringe phaser sensitivity for unresolved targets will be K- 22.0, 20.0 and 17.9 on the K-K, K-O and O-O baselines, respectively. Synthetic imaging capability will be available in the 1.6-10.0 micrometers atmospheric transmission bands at angular resolutions of 4.0 milli-arcseconds. In this article, we briefly outline the adopted methodology, imaging hardware, projected sensitivities and summarize the scientific potential of the instrument as an imaging interferometer.
© (1998) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Gautam Vasisht, Andrew F. Boden, M. Mark Colavita, Samuel L. Crawford, Michael Shao, Paul N. Swanson, Gerard Theodore van Belle, J. Kent Wallace, James M. Walker, and Peter L. Wizinowich "Aperture synthesis imaging with the Keck Interferometer", Proc. SPIE 3350, Astronomical Interferometry, (24 July 1998); doi: 10.1117/12.317097; https://doi.org/10.1117/12.317097


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