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Recent astronomical results from the infrared spatial interferometer and their implications for LOUISAA new heterodyne interferometer for the atmospheric window from 9 to 12 microns was developed during the past five years. This instrument, called the Infrared Spatial Interferometer (ISI), was designed to use earth rotation aperture synthesis techniques developed in radio interferometry. It was moved to Mt. Wilson, California, in January 1988 and first fringes were obtained in June of that year. Systematic observations of some of the brighter late-type stars began shortly after the first fringes were obtained. We describe the basic principles and design of the ISI and give an overview of some of the initial results obtained from these observations. The implications of our work to the proposed Lunar Optical/UV/IR Synthesis Array (LOUISA) are discussed. We also analyze the conditions for the maximum signal-to-noise ratio of such an interferometer as a function of wavelength. The optimum wavelength is found to depend on the assumed scaling relation between telescope area and wavelength.
Document ID
19930004397
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Danchi, William C.
(California Univ. Berkeley, CA, United States)
Bester, M.
(California Univ. Berkeley, CA, United States)
Townes, C. H.
(California Univ. Berkeley, CA, United States)
Date Acquired
September 6, 2013
Publication Date
November 1, 1992
Publication Information
Publication: New Mexico Univ., A Lunar Optical-Ultraviolet-Infrared Synthesis Array (LOUISA)
Subject Category
Astronomy
Accession Number
93N13585
Funding Number(s)
CONTRACT_GRANT: N00014-82-C-0700
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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