Review of the state of infrared detectors for astronomy in retrospect of the June 2002 workshop on scientific detectors for astronomy
Review of the state of infrared detectors for astronomy in retrospect of the June 2002 workshop on scientific detectors for astronomy
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回顾 2002 年 6 月天文学科学探测器研讨会，回顾天文学红外探测器的现状
DOI：
10.1117/12.462593
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发表时间：
2003
期刊：
影响因子：
--
通讯作者：
J. Beletic
中科院分区：
文献类型：
--
作者：
G. Finger;J. Beletic
就在两个月前，即 2002 年 6 月，天文学科学探测器研讨会在威美亚举行，工作在焦平面技术前沿的光学 CCD 和红外探测器专家首次齐聚一堂。光学探测器（例如 CCD 和 CMOS 器件）的新发展概述将在本会议的其他部分进行概述。本文将重点关注欧洲南方天文台 ESO 进行的红外探测器开发，还将包括威美亚研讨会上介绍的红外焦平面技术的精选亮点。地面天文学家的三个主要探测器开发目前正在推动红外焦平面技术。在 1 至 5 μm 的近红外区域，将审查两种技术，即通过 LPE 或 MBE 在 Al2O3、Si 或 CdZnTe 基板上生长的 InSb 和 HgCdTe，这两种技术均旨在实现可对接的 2K x 2K 镶嵌。阻挡杂质带 Si:As 阵列覆盖 8 至 28 μm 的中红外光谱范围。由于红外阵列的视频信号与 CCD 不同，是直流耦合的，因此红外阵列的长时间曝光极易受到漂移和低至 mHz 范围的低频噪声拾取的影响。将讨论利用片上参考像素减少热漂移和抑制低频噪声的新技术。将指出开发用于自适应光学和干涉测量的小型低噪声传感器的必要性。
Only two months ago, in June 2002, a workshop on scientific detectors for astronomy was held in Waimea, where for the first time both experts on optical CCD's and infrared detectors working at the cutting edge of focal plane technology gathered. An overview of new developments in optical detectors such as CCD's and CMOS devices will be given elsewhere in these proceedings. This paper will focus on infrared detector developments carried out at the European Southern Observatory ESO and will also include selected highlights of infrared focal plane technology as presented at the Waimea workshop. Three main detector developments for ground based astronomers are currently pushing infrared focal plane technology. In the near infrared from 1 to 5 μm two technologies, both aiming for buttable 2K x 2K mosaics, will be reviewed, namely InSb and HgCdTe grown by LPE or MBE on Al2O3, Si or CdZnTe substrates. Blocked impurity band Si:As arrays cover the mid infrared spectral range from 8 to 28 μm. Since the video signal of infrared arrays, contrary to CCD's, is DC coupled, long exposures with IR arrays are extremely susceptible to drifts and low frequency noise pick-up down to the mHz regime. New techniques to reduce thermal drifts and suppress low frequency nosie with on-chip reference pixels will be discussed. The need for the development of small format low noise sensors for adaptive optics and interferometry will be pointed out.