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20 October 1993 Near-infrared arrays for SIRTF, the Space Infrared Telescope Facility
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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.
© (1993) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
William J. Forrest, Hao Chen, James D. Garnett, Steven Lawrence Solomon, and Judith L. Pipher "Near-infrared arrays for SIRTF, the Space Infrared Telescope Facility", Proc. SPIE 1946, Infrared Detectors and Instrumentation, (20 October 1993);


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