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

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

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993spie.1946...18f&link_type=abstract

Proc. SPIE Vol. 1946, p. 18-24, Infrared Detectors and Instrumentation, Albert M. Fowler; Ed.

Computer Science

Performance

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Scientific paper

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(superscript -)/s/pixel. The detector noise must be less than the noise given by fluctuations in the number of zodiacal background photons (< 9 e(superscript -)/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.

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