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Infrared Detector For Mid-Infrared Astronomy
Astrophysics and Space Science, 1989Recent developments of infrared detectors and arrays for mid-infrared astronomical observations are discussed with an emphasis on technical issues in designing and fabricating photometers and cameras. The discussion includes a small-scale silicon bolometer array being tested at the Steward Observatory.
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Immersion grating for infrared astronomy
Applied Optics, 1993An immersion grating with high refractive index n increases spectral resolution n-fold over that of a surface reflection grating of equal length.
G, Wiedemann, D E, Jennings
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Infrared Astronomy Instruments
Optical Engineering, 1977In this issue devoted to Infrared Astronomy Instruments, you will note that most of the instruments are designed for use at altitude, either in aircraft, balloons, probes or satellites. Such usage permits observation above the interfering atmosphere usually encountered during ground observations.
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Instrumentation for Infrared Astronomy
Annual Review of Astronomy and Astrophysics, 1978Over the last 10 years infrared astronomy from 2 µm to 1000 µm has blossomed into a major field of observational astrophysics. This development would have been impossible without two major technical advances. First, extremely sensitive detectors have been developed and become available for astronomical applications.
Soifer, B. T., Pipher, Judith L.
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Publications of the Astronomical Society of Australia, 1977
Infrared astronomical observations using ground-based equipment are confined to the few ‘windows’ or observation ports allowed by our absorbing atmosphere, the chief absorbing molecules being water vapour and CO2. The majority of such observations have been made using broadband filters defining the photometric J, H, K, L, M, N and O bands.
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Infrared astronomical observations using ground-based equipment are confined to the few ‘windows’ or observation ports allowed by our absorbing atmosphere, the chief absorbing molecules being water vapour and CO2. The majority of such observations have been made using broadband filters defining the photometric J, H, K, L, M, N and O bands.
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Publications of the Astronomical Society of Australia, 1971
Until the last six years few infrared observations of astronomical objects (other than the Sun and planets) had been attempted. Those few were primarily concerned with obtaining bolometric corrections and effective temperatures, the variation of bolometric magnitudes of late-type variables, and the derivation of the laws of interstellar extinction.
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Until the last six years few infrared observations of astronomical objects (other than the Sun and planets) had been attempted. Those few were primarily concerned with obtaining bolometric corrections and effective temperatures, the variation of bolometric magnitudes of late-type variables, and the derivation of the laws of interstellar extinction.
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1971
Abstract : The report describes the work completed between 11 December 1970 and 10 May 1971, and is divided into seven sections; performance of the reassembled telescope system, the new optical system, results of December 2, 1970 flight: short wavelength detectors, results of December 2, 1970 flight: long wavelength detectors, ground based effort ...
Baruch T. Soifer +4 more
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Abstract : The report describes the work completed between 11 December 1970 and 10 May 1971, and is divided into seven sections; performance of the reassembled telescope system, the new optical system, results of December 2, 1970 flight: short wavelength detectors, results of December 2, 1970 flight: long wavelength detectors, ground based effort ...
Baruch T. Soifer +4 more
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Stellar infrared astronomy with EDISON
Space Science Reviews, 1992In this review the IR emission from circumstellar material is discussed, both of ionized gas and dust grains, and the astrophysical information that can be extracted from such observations. Some emphasis is placed on the possibilities of stellar IR astronomy using a large space-borne telescope, especially with respect to the much better spatial and ...
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1972
The extension of astronomy in the wavelength region of 1 μ to 1 mm has in the past been limited by lack of detectors of high sensitivity and by the obscuration of the Earth’s atmosphere. Ground-based near infrared astronomy could be carried out within certain partial windows: i.e. from 2.1 μ to 2.4 μ, 3.5 μ to 4.0 μ, 4.6 μ to 4.7 μ, 8–13 μ, and 20–25 μ.
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The extension of astronomy in the wavelength region of 1 μ to 1 mm has in the past been limited by lack of detectors of high sensitivity and by the obscuration of the Earth’s atmosphere. Ground-based near infrared astronomy could be carried out within certain partial windows: i.e. from 2.1 μ to 2.4 μ, 3.5 μ to 4.0 μ, 4.6 μ to 4.7 μ, 8–13 μ, and 20–25 μ.
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