Infrared detector development programs for the VLT instruments at the European Southern Observatory
Infrared detector development programs for the VLT instruments at the European Southern Observatory
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欧洲南方天文台 VLT 仪器的红外探测器开发计划
DOI：
10.1117/12.317209
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发表时间：
1998
期刊：
影响因子：
--
通讯作者：
J. Stegmeier
中科院分区：
文献类型：
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作者：
G. Finger;P. Biereichel;Hamid Mehrgan;M. Meyer;A. Moorwood;G. Nicolini;J. Stegmeier
像VLT这样的仪器平台对红外焦平面技术提出了新的挑战。由于大望远镜直径和自适应光学提供的改善的图像质量减小了像素尺度，因此需要更大的阵列格式。为了迎接这一挑战，ESO正在参与InSb和HgCdTe大格式阵列的开发计划。为了覆盖1到5微米的光谱区域，ESO资助了SBRC的一次代工运行，以生产1024×1024 InSb阵列，该阵列将安装在为VLT制造的红外光谱仪和阵列相机Isaac上。由于1K×1K InSb阵列的交付延迟，将讨论256×256 InSb阵列的测试结果以及片外低温放大器在InSb探测器中的应用。给出了用等于2.5微米的罗克韦尔1024×1024 HgCdTe阵列获得的结果，其中使用了一个片外低温运算放大器，产生了3个电子的均方根读取噪声。用单模红外光纤测量了单个像素的灵敏度分布。将讨论Pace 1技术的局限性，如持久性。首先将介绍安装在SOFI的1K×1K阵列的结果，该阵列是在NTT望远镜上提供1-2.5微米成像和长缝棱镜光谱的红外减焦器。先进的实时图像锐化技术也将包括在内。展望了(Lambda)c=2048×2048 HgCdTe阵列格式的发展前景。NIRMOS是一种用于VLT望远镜的多目标光谱仪，其光学布局是基于2K×2K HgCdTe阵列的可用性。
Instrument platforms like the VLT represent a new challenge to IR focal plane technology. Since the large telescope diameter and the improved image quality provided by adaptive optics reduce the pixel scale, larger array formats are needed. To meet this challenge ESO is participating in development programs for both InSb and HgCdTe large format arrays. To cover the spectral region of 1 to 5 micron ESO has funded a foundry run at SBRC to produce 1024 X 1024 InSb arrays, which will be installed in ISAAC, the IR Spectrometer and Array Camera built for the VLT. Since the delivery of the 1K X 1K InSb array is delayed, the test results obtained with a 256 X 256 InSb array and the application of off chip cryogenic amplifiers to InSb detectors will be discussed. Results obtained with a (lambda) c equals 2.5 micrometers Rockwell 1024 X 1024 HgCdTe array will be presented, where an off chip cryogenic operational amplifier was used yielding a rms read noise of 3 electrons. Sensitivity profiles of individual pixels have been measured with a single mode IR fiber. Limitations of PACE 1 technology, such as persistence, will be discussed. First results with the 1K X 1K array, which was installed in SOFI, an IR focal reducer providing 1-2.5 micron imaging and long slit grism spectroscopy at the NTT telescope, will be presented. Advanced techniques of real time image sharpening will also be included. An outlook to the development of (lambda) c equals 2048 X 2048 HgCdTe array formats will be given. The optical layout of NIRMOS, a multi-object spectrograph for the VLT telescope, is base don the availability of 2K X 2K HgCdTe arrays.