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Low-loss photonic Nulling Interferometer in the Mid-Infrared for Astronomical Applications
Frontiers in Optics 2017, 2017Thomas Gretzinger, Peter G. Tuthill
exaly +2 more sources
Stellar Interferometer for Figure Sensing of Orbiting Astronomical Telescopes
Applied Optics, 1974An interferometric device designed to be located in the focal plane of a large astronomical telescope is presented. The prime application is for the forthcoming large space telescope. The device is to perform interferometry on the optical wavefront arising from a single star after it has propagated through the telescope.
W N, Peters, R A, Arnold, S, Gowrinathan
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A HELIUM COOLED FABRY–PEROT INTERFEROMETER FOR INFRARED ASTRONOMICAL SPECTROSCOPY
Infrared Physics, 1976Abstract We have built a cooled, scanning Fabry-Perot interferometer for astronomical spectroscopy in the ten micron atmospheric window. The reasons for choosing this approach are discussed and details are given of the construction and performance of the prototype instrument.
M.J. Selby, P.R. Jorden, A.D. MacGregor
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A cryogenic tunable Fabry-Perot interferometer for astronomical observations
SPIE Proceedings, 2007The Lockheed Martin - University of Arizona Infrared Spectrometer (LAIRS) is designed to image the emission lines of celestial objects in the 1.3-2.5 μm regime. The Instrument has been built and tested at the Lockheed Martin Space Systems Advanced Technology Center, and demonstrated to work at cryogenic temperatures. The Instrument employs a tunable
Jonathan K. Chow +4 more
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Development of bolometric astronomical interferometer in mm and submm bands
2005 Joint 30th International Conference on Infrared and Millimeter Waves and 13th International Conference on Terahertz Electronics, 2006We are developing a bolometric astronomical interferometer in mm and submm wave bands by applying Martin-Puplett type Fourier transform spectrometer to aperture synthesis technique. Since the spectroscopically resolved intensity distribution of four Stokes parameters are measurable by this instrument, we refer this to multi-components Fourier transform
M. Hattori +3 more
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Superconducting electromagnetic actuators for astronomical Fabry-Perot interferometers
IEEE Transactions on Magnetics, 1985Two types of superconducting electromagnetic actuators-linear and angular-for precise control of Fabry-Perot spectrometer etalons at liquid helium temperature were manufactured and tested successfully. The linear displacement unit (45 Newtons/Amp) has maximum travel of ±44 um with off-axis deviation of less than 1.5 arcseconds for 15 um path.
T. Nishimura, F. Low, K. Shivanandan
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Astronomical Infrared Spectroscopy with a Connes-Type Interferometer. I. Instrumental
Review of Scientific Instruments, 1971The construction and operation of a Connes-type Fourier spectrometer are discussed in an astronomical context with a sample of the type of spectra obtained with the system.
Reinhard Beer +2 more
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Towards an ultrafast laser inscribed astronomical nulling interferometer in the mid-infrared
2017 Conference on Lasers and Electro-Optics Europe & European Quantum Electronics Conference (CLEO/Europe-EQEC), 2017One of the biggest challenges in modem Astronomy is the direct detection of extrasolar planets using ground based telescopes. While the small angular separation of the star-planet system is an unchangeable limitation, the contrast ratio can dramatically be improved by shifting the observing wavelength to the mid-infrared. In the astronomical L'-band (3.
Thomas Gretzinger +4 more
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Astronomical, Atmospheric, and Wavefront Studies with a Submillimeter-wavelength Interferometer
1996Over the course of the last half century, astrophysical investigations have expanded into ever wider sections of the electromagnetic spectrum. One of the most difficult wavebands to access, both for atmospheric and technological reasons, is the submillimeter band, between wavelengths of roughly 1 mm and 100 fim.
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Radiophysics and Quantum Electronics, 1979
1) Equations (8) imply that the variances of the correction estimates of the direction of the baseline Bi are independent of the configuration of the interferometer elements which do not constitute Bi, but they do depend on the number m+1. This fact can explain why the optimal measurement procedure requires the calculation of correlation functions ...
P. Yu. Kostenko +2 more
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1) Equations (8) imply that the variances of the correction estimates of the direction of the baseline Bi are independent of the configuration of the interferometer elements which do not constitute Bi, but they do depend on the number m+1. This fact can explain why the optimal measurement procedure requires the calculation of correlation functions ...
P. Yu. Kostenko +2 more
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