The Space Telescope Imaging Spectrograph Design
The Space Telescope Imaging Spectrograph Design
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DOI：
10.1086/316243
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发表时间：
1998-10
影响因子：
3.5
通讯作者：
B. Woodgate;R. Kimble;C. Bowers;S. Kraemer;M. Kaiser;A. Danks;J. Grady;J. Loiacono;M. Brumfield;L. Feinberg;T. Gull;S. Heap;S. Maran;D. Lindler;D. Hood;W. Meyer;C. VanHouten;V. Argabright;Steven Franka;R. L. Bybee;D. Dorn;M. Bottema;R. Woodruff;D. Michika;J. Sullivan;J. Hetlinger;C. W. Ludtke;R. Stocker;A. Delamere;D. Rose;I. Becker;H. Garner;J. Timothy;M. Blouke;C. Joseph;G. Hartig;R. Green;E. Jenkins;J. Linsky;J. Hutchings;H. Moos;A. Boggess;F. Roesler;D. Weistrop
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文献类型：
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作者：
B. Woodgate;R. Kimble;C. Bowers;S. Kraemer;M. Kaiser;A. Danks;J. Grady;J. Loiacono;M. Brumfield;L. Feinberg;T. Gull;S. Heap;S. Maran;D. Lindler;D. Hood;W. Meyer;C. VanHouten;V. Argabright;Steven Franka;R. L. Bybee;D. Dorn;M. Bottema;R. Woodruff;D. Michika;J. Sullivan;J. Hetlinger;C. W. Ludtke;R. Stocker;A. Delamere;D. Rose;I. Becker;H. Garner;J. Timothy;M. Blouke;C. Joseph;G. Hartig;R. Green;E. Jenkins;J. Linsky;J. Hutchings;H. Moos;A. Boggess;F. Roesler;D. Weistrop
空间望远镜成像光谱仪(STIS)仪器在1997年2月的第二次维修任务中安装在哈勃空间望远镜(HST)上。四个波段覆盖115-1000 nm的波长范围，光谱分辨率在26-200,000之间。相机模式用于目标捕获和深度成像。包括对HST的球差和散光的校正。115-170 nm范围由CSI MAMA(多阳极微通道阵列)探测器覆盖，165-310 nm范围由Cs2Te MAMA覆盖，每个MAMA的格式为2048×2048像素，而305-555和550-1000 nm范围由格式为1024×1024像素的单个CCD覆盖。与第一代摄谱仪的1×512像素探测器相比，使用这些二维探测器的多路复用优势是1或2个数量级，具体取决于所使用的模式。讨论了科学目标与仪器规格和设计之间的关系。
The Space Telescope Imaging Spectrograph (STIS) instrument was installed on the Hubble Space Telescope (HST) during the second servicing mission, in 1997 February. Four bands cover the wavelength range of 115–1000 nm, with spectral resolving powers between 26 and 200,000. Camera modes are used for target acquisition and deep imaging. Correction for HST's spherical aberration and astigmatism is included. The 115–170 nm range is covered by a CsI MAMA (Multianode Microchannel Array) detector and the 165–310 nm range by a Cs2Te MAMA, each with a format of 2048 × 2048 pixels, while the 305–555 and 550–1000 nm ranges are covered by a single CCD with a format of 1024 × 1024 pixels. The multiplexing advantage of using these two‐dimensional detectors compared with the 1 × 512 pixel detectors of the first‐generation spectrographs is 1 or 2 orders of magnitude, depending on the mode used. The relationship between the scientific goals and the instrument specifications and design is discussed.