2K X 2K HgCdTe detector arrays for VISTA and other applications

Peter J. Love; Alan W. Hoffman; Ken J. Ando; Elizabeth Corrales; William D. Ritchie; Neil J. Therrien; Joseph P. Rosbeck; Roger S. Holcombe; David J. Gulbransen

doi:10.1117/12.555225

29 September 2004 2Kx2K HgCdTe detector arrays for VISTA and other applications

Peter J. Love, Alan W. Hoffman, Ken J. Ando, Elizabeth Corrales, William D. Ritchie, Neil J. Therrien, Joseph P. Rosbeck, Roger S. Holcombe, David J. Gulbransen

Author Affiliations +

Proceedings Volume 5499, Optical and Infrared Detectors for Astronomy; (2004) https://doi.org/10.1117/12.555225
Event: SPIE Astronomical Telescopes + Instrumentation, 2004, Glasgow, United Kingdom

Abstract

The demand for large-format near infrared arrays has grown for both ground-based and space-based applications. These arrays are required for maintaining high resolution over very large fields of view for survey work. We describe results of the development of a new 2048 × 2048 HgCdTe/CdZnTe array with 20-micron pixels that responds with high quantum efficiency over the wavelength range 0.85 to 2.5 microns. With a single-layer anti-reflection coating, the responsive quantum efficiency is greater than 70% from 0.9 micron to 2.4 microns. Dark current is typically less than 4 e-/sec at 80 K. The modular package for this array, dubbed the VIRGO array, allows 3-side butting to form larger mosaic arrays of 4K × 2nK format. The VIRGO ROIC utilizes a PMOS Source Follower per Detector input circuit with a well capacity of about 2 × 10⁵ electrons and with a read noise of less than 20 e- rms with off-chip Correlated Double Sampling. Other features of the VIRGO array include 4 or 16 outputs (programmable), and a frame rate of up to 1.5 Hz in 16-output mode. Power dissipation is about 7 mW at a 1 Hz frame rate. Reset modes include both global reset and reset by row (ripple mode). Reference pixels are built-in to the output data stream. The first major application of the VIRGO array will be for VISTA, the United Kingdom’s Visible and Infrared Survey Telescope for Astronomy. The VISTA focal plane array will operate near 80 K. The cutoff wavelength of the HgCdTe detector can be adjusted for other applications such as SNAP, the Supernova/Acceleration Probe, which requires a shorter detector cutoff wavelength of about 1.7 microns. For applications which require both visible and near infrared response, the detector CdZnTe substrate can be removed after hybridization, allowing the thinned detector to respond to visible wavelengths as short as 0.4 microns.

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Peter J. Love, Alan W. Hoffman, Ken J. Ando, Elizabeth Corrales, William D. Ritchie, Neil J. Therrien, Joseph P. Rosbeck, Roger S. Holcombe, and David J. Gulbransen "2Kx2K HgCdTe detector arrays for VISTA and other applications", Proc. SPIE 5499, Optical and Infrared Detectors for Astronomy, (29 September 2004); https://doi.org/10.1117/12.555225

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