Aperture synthesis imaging with the Keck interferometer

被引：8

作者：

Vasisht, G ^{[1
]}

Boden, AF ^{[1
]}

Colavita, MM ^{[1
]}

Crawford, SL ^{[1
]}

Shao, M ^{[1
]}

Swanson, P ^{[1
]}

van Belle, GT ^{[1
]}

Wallace, JK ^{[1
]}

Walker, JM ^{[1
]}

Wizinowich, PL ^{[1
]}

机构：

[1] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

来源：

ASTRONOMICAL INTERFEROMETRY, PTS 1 AND 2 | 1998年 / 3350卷

关键词：

interferometry; SPIE Proceedings; Keck; synthesis imaging;

D O I：

10.1117/12.317097

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

JPL and CARA are building a multi-element, infrared interferometer for NASA to be situated at the twin Keck Observatories on Mauna Kea, Hawaii. Initially, the IO-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 similar or equal to 110 m or nearly 5 x 10(7) (lambda/2.2 mu m)(-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 cc-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 phasor sensitivity for unresolved targets will be K similar to 22.0, 20.0 and 17.9 (10-sigma in 10(3) s) on the K-K, K-O and O-O baselines, respectively Synthetic imaging capability will be available in the 1.6 - 10.0 mu m atmospheric transmission bands at angular resolutions of 4.0(lambda/2.2 mu m) 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.

引用

页码：354 / 361

页数：8