2Kx2K HgCdTe detector arrays for VISTA and other applications
2Kx2K HgCdTe detector arrays for VISTA and other applications
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适用于 VISTA 和其他应用的 2Kx2K HgCdTe 探测器阵列
DOI：
10.1117/12.555225
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发表时间：
2004
期刊：
影响因子：
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通讯作者：
D. Gulbransen
中科院分区：
文献类型：
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作者：
P. Love;A. Hoffman;K. J. Ando;E. Corrales;W. Ritchie;N. Therrien;J. Rosbeck;Roger S. Holcombe;D. Gulbransen
地面和天基应用对大画幅近红外阵列的需求都在增长。这些阵列需要在非常大的视场上保持高分辨率来进行测量工作。我们描述了一种具有20微米像素的新型2048 × 2048 HgCdTe/CdZnTe阵列的开发结果，该阵列在0.85至2.5微米的波长范围内具有高量子效率。采用单层增透涂层，从0.9微米到2.4微米的响应量子效率大于70%。在80k时，暗电流通常小于4 e-/秒。该阵列的模块化封装，被称为VIRGO阵列，允许3面对接，形成更大的4K × 2nK格式的马赛克阵列。VIRGO ROIC采用每个检测器输入电路的PMOS源跟随器，容量约为2 × 105个电子，片外相关双采样的读取噪声小于20 e- rms。VIRGO阵列的其他特点包括4个或16个输出（可编程），在16输出模式下帧率高达1.5 Hz。在1hz帧率下，功耗约为7mw。重置模式包括全局重置和行重置（波纹模式）。参考像素是内置到输出数据流中的。处女座阵列的第一个主要应用将是英国的可见光和红外天文巡天望远镜VISTA。VISTA焦平面阵列将在80k附近工作。HgCdTe探测器的截止波长可以根据其他应用进行调整，如超新星/加速探测器SNAP，这需要更短的探测器截止波长，约为1.7微米。对于需要可见光和近红外响应的应用，探测器CdZnTe衬底可以在杂化后去除，使薄化的探测器能够响应短至0.4微米的可见光。
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.