The Keck Interferometer

被引：30

作者：

Colavita, M. M. ^{[1
]}

Wizinowich, P. L. ^{[2
]}

Akeson, R. L. ^{[3
]}

Ragland, S. ^{[2
]}

Woillez, J. M. ^{[2
]}

Millan-Gabet, R. ^{[3
]}

Serabyn, E. ^{[1
]}

Abajian, M. ^{[3
]}

Acton, D. S. ^{[2
]}

Appleby, E. ^{[2
]}

Beletic, J. W. ^{[2
]}

Beichman, C. A. ^{[3
]}

Bell, J. ^{[2
]}

Berkey, B. C. ^{[2
]}

Berlin, J. ^{[1
]}

Boden, A. F. ^{[3
]}

Booth, A. J. ^{[1
]}

Boutell, R. ^{[2
]}

Chaffee, F. H. ^{[2
]}

Chan, D. ^{[2
]}

Chin, J. ^{[2
]}

Chock, J. ^{[2
]}

Cohen, R. ^{[2
]}

Cooper, A. ^{[2
]}

Crawford, S. L. ^{[1
]}

Creech-Eakman, M. J. ^{[1
]}

Dahl, W. ^{[2
]}

Eychaner, G. ^{[1
]}

Fanson, J. L. ^{[1
]}

Felizardo, C. ^{[3
]}

Garcia-Gathright, J. I. ^{[1
]}

Gathright, J. T. ^{[2
]}

Hardy, G. ^{[1
]}

Henderson, H. ^{[3
]}

Herstein, J. S. ^{[3
]}

Hess, M. ^{[2
]}

Hovland, E. E. ^{[1
]}

Hrynevych, M. A. ^{[2
]}

Johansson, E. ^{[2
]}

Johnson, R. L., Jr. ^{[1
]}

Kelley, J. ^{[1
]}

Kendrick, R. ^{[2
]}

Koresko, C. D. ^{[3
]}

Kurpis, P. ^{[2
]}

Le Mignant, D. ^{[2
]}

Lewis, H. A. ^{[2
]}

Ligon, E. R. ^{[1
]}

Lupton, W. ^{[2
]}

McBride, D. ^{[2
]}

Medeiros, D. W. ^{[2
]}

机构：

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

[2] Calif Assoc Res Astron, WM Keck Observ, Kamuela, HI 96743 USA

[3] CALTECH, NASA Exoplanet Sci Ctr, Pasadena, CA 91125 USA

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 2013年 / 125卷 / 932期

基金：

美国国家航空航天局; 美国国家科学基金会;

关键词：

Astronomical Instrumentation; PALOMAR TESTBED INTERFEROMETER; NARROW-ANGLE ASTROMETRY; ADAPTIVE OPTICS SYSTEM; INFRARED INTERFEROMETRY; VISIBILITY ESTIMATORS; II TELESCOPE; WATER-VAPOR; NULLER; PERFORMANCE; PROGRESS;

D O I：

10.1086/673475

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Keck Interferometer (KI) combined the two 10m W. M. Keck Observatory telescopes on Mauna Kea, Hawaii, as a long-baseline near- and mid-infrared interferometer. Funded by NASA, it operated from 2001 until 2012. KI used adaptive optics on the two Keck telescopes to correct the individual wavefronts, as well as active fringe tracking in all modes for path-length control, including the implementation of cophasing to provide long coherent integration times. KI implemented high sensitivity fringe-visibility measurements at H (1.6m), K (2.2m), and L (3.8m) bands, and nulling measurements at N band (10m), which were used to address a broad range of science topics. Supporting these capabilities was an extensive interferometer infrastructure and unique instrumentation, including some additional functionality added as part of the NSF-funded ASTRA program. This paper provides an overview of the instrument architecture and some of the key design and implementation decisions, as well as a description of all of the key elements and their configuration at the end of the project. The objective is to provide a view of KI as an integrated system, and to provide adequate technical detail to assess the implementation. Included is a discussion of the operational aspects of the system, as well as of the achieved system performance. Finally, details on V-2 calibration in the presence of detector nonlinearities as applied in the data pipeline are provided.

引用

页码：1226 / 1264

页数：39

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