Near-infrared arrays for SIRTF, the Space Infrared Telescope Facility

William J. Forrest; Hao Chen; James D. Garnett; Steven Lawrence Solomon; Judith L. Pipher

doi:10.1117/12.158680

20 October 1993 Near-infrared arrays for SIRTF, the Space Infrared Telescope Facility

William J. Forrest, Hao Chen, James D. Garnett, Steven Lawrence Solomon, Judith L. Pipher

Proceedings Volume 1946, Infrared Detectors and Instrumentation; (1993) https://doi.org/10.1117/12.158680
Event: Optical Engineering and Photonics in Aerospace Sensing, 1993, Orlando, FL, United States

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.

Citation Download Citation

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); https://doi.org/10.1117/12.158680

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