The photodetector array camera and spectrometer (PACS) for the Herschel Space Observatory
The photodetector array camera and spectrometer (PACS) for the Herschel Space Observatory
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赫歇尔空间天文台的光电探测器阵列相机和光谱仪 (PACS)
DOI：
10.1117/12.670654
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发表时间：
2006
影响因子：
4.8
通讯作者：
B. Vandenbussche
中科院分区：
文献类型：
--
作者：
A. Poglitsch;C. Waelkens;O. Bauer;J. Cepa;H. Feuchtgruber;T. Henning;C. van Hoof;F. Kerschbaum;D. Lemke;E. Renotte;L. Rodriguez;P. Saraceno;B. Vandenbussche
光电探测器阵列相机和光谱仪（PACS）是欧空局远红外和亚毫米波天文台赫歇尔的三个科学仪器之一。它采用两个16 × 25像素的Ge：Ga光电导体阵列（应力和非应力）和两个分别为16 × 32和32 × 64像素的填充硅测辐射热计阵列，在60-210μm波段进行成像线光谱和成像测光。在测光模式下，它将同时成像两个波段，60-85μm或85-130μm和130-210μm，视场约为1.75' × 3.5'，每个波段都有全光束采样。在光谱模式下，它将对~50”×50”的区域成像，分辨率为5×5像素，瞬时光谱覆盖范围为~1500 km/s，光谱分辨率为~ 175 km/s。在这两种模式下，性能预计不会远离背景噪声限制，灵敏度（5σ在1小时内）分别为~ 4 mJy或3 - 20 ×10- 18 W/m2。我们总结了仪器及其子单元的设计，结合望远镜指向模式描述了观测模式，报告了合格模型的仪器级性能测试结果，并根据在子单元级进行的测试，提出了我们目前对仪器在轨性能的预测。
The Photodetector Array Camera and Spectrometer (PACS) is one of the three science instruments for ESA's far infrared and submillimeter observatory Herschel. It employs two Ge:Ga photoconductor arrays (stressed and unstressed) with 16 × 25 pixels, each, and two filled silicon bolometer arrays with 16 × 32 and 32 × 64 pixels, respectively, to perform imaging line spectroscopy and imaging photometry in the 60-210μm wavelength band. In photometry mode, it will simultaneously image two bands, 60-85μm or 85-130μm and 130-210μm, over a field of view of ~ 1.75' × 3.5', with full beam sampling in each band. In spectroscopy mode, it will image a field of ~50"×50", resolved into 5×5 pixels, with an instantaneous spectral coverage of ~1500 km/s and a spectral resolution of ~ 175 km/s. In both modes the performance is expected to be not far from background-noise limited, with sensitivities (5σ in 1h) of ~ 4 mJy or 3 - 20 ×10-18W/m2, respectively. We summarize the design of the instrument and its subunits, describe the observing modes in combination with the telescope pointing modes, report results from instrument level performance tests of the Qualification Model, and present our current prediction of the in-orbit performance of the instrument based on tests done at subunit level.