16 September 2011 Evolution of large format impurity band conductor focal plane arrays for astronomy applications
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Abstract
Raytheon Vision Systems (RVS) has developed a family of high performance large format infrared (IR) detector arrays whose detectors are most effective for the detection of long and very long wavelength IR energy. This paper describes the evolution of the present state of the art one mega-pixel Si: As Impurity Band Conduction (IBC) arrays toward a four mega-pixel array that is desired by the astronomy community. Raytheon's Aquarius-1k, developed in collaboration with ESO, is a 1024 × 1024 pixel high performance array with a 30 μm pitch that features high quantum efficiency IBC detectors, low noise, low dark current, and on-chip clocking for ease of operation. Since the Aquarius-1k array was designed primarily for ground-based astronomy applications, it incorporates selectable gains and a large well capacity among its other features. Raytheon, in collaboration with JAXA (Japan Aerospace Exploration Agency), is also designing a 2048 × 2048 pixel high performance array with a 25 μm pitch. This 2k × 2k readout circuit will be based on the successful design used for the on the Mid-Infrared Instrument (MIRI) aboard the James Webb Space Telescope (JWST). It will feature high quantum efficiency IBC detectors, low noise, low dark current, and on-chip clocking for ease of operation. This version will also incorporate flight qualified packaging to support space-based astronomy applications. Previous generations of RVS IBC detectors have flown on several platforms, including NASA's Spitzer Space Telescope and Japan's Akari Space Telescope.
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Robert Mills, Robert Mills, Eric Beuville, Eric Beuville, Elizabeth Corrales, Elizabeth Corrales, Alan Hoffman, Alan Hoffman, Gert Finger, Gert Finger, Derek Ives, Derek Ives, } "Evolution of large format impurity band conductor focal plane arrays for astronomy applications", Proc. SPIE 8154, Infrared Remote Sensing and Instrumentation XIX, 81540R (16 September 2011); doi: 10.1117/12.897292; https://doi.org/10.1117/12.897292
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