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Proceedings Paper

Near-infrared arrays for SIRTF, the Space Infrared Telescope Facility
Author(s): William J. Forrest; Hao Chen; James D. Garnett; Steven Lawrence Solomon; Judith L. Pipher
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Paper Abstract

SIRTF, and other infrared space astronomy projects, require detector arrays with extremely high sensitivity. It is a goal of SIRTF to achieve background limited performance at all wavelengths. Especially critical is the spectral region around 3 micrometers , where the detector current due to the zodiacal background radiation is a minimum. For background limited operation, at a spectral resolution of 100, the dark current must be less than 0.1 e-/s/pixel. The detector noise must be less than the noise given by fluctuations in the number of zodiacal background photons (< 9 e-/pixel). Other detector array goals include: high quantum efficiency (> 90%), radiation hardness, minimal image latency, and excellent photometric accuracy and stability. Many of the performance goals have been met with Santa Barbara Research Center's 256 X 256 InSb arrays.

Paper Details

Date Published: 20 October 1993
PDF: 7 pages
Proc. SPIE 1946, Infrared Detectors and Instrumentation, (20 October 1993); doi: 10.1117/12.158680
Show Author Affiliations
William J. Forrest, Univ. of Rochester (United States)
Hao Chen, Univ. of Rochester (United States)
James D. Garnett, Univ. of Rochester (United States)
Steven Lawrence Solomon, Univ. of Rochester (United States)
Judith L. Pipher, Univ. of Rochester (United States)


Published in SPIE Proceedings Vol. 1946:
Infrared Detectors and Instrumentation
Albert M. Fowler, Editor(s)

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