PEPSI: The high-resolution ichelle spectrograph and polarimeter for the Large Binocular Telescope
PEPSI: The high-resolution ichelle spectrograph and polarimeter for the Large Binocular Telescope
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PEPSI：大型双目望远镜的高分辨率米歇尔摄谱仪和旋光仪
DOI：
10.1002/asna.201512172
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发表时间：
2015
影响因子：
0.9
通讯作者：
J. Storm
中科院分区：
文献类型：
--
作者：
K. Strassmeier;I. Ilyin;A. Jarvinen;M. Weber;M. Woche;S. Barnes;S. Bauer;E. Beckert;W. Bittner;R. Bredthauer;T. Carroll;C. Denker;F. Dionies;I. DiVarano;D. Doscher;T. Fechner;D. Feuerstein;T. Granzer;T. Hahn;G. Harnisch;A. Hofmann;M. Lesser;J. Paschke;S. Pankratow;V. Plank;D. Pluschke;E. Popow;D. Sablowski;J. Storm
PEPSI是用于2×8.4米大双筒望远镜（LBT）的台式、双臂、光纤馈电和稳定的波茨坦中阶梯偏振和光谱仪器。三个光谱分辨率的43 000，120 000或270 000可以覆盖整个光学/红色波长范围从383至907 nm在三次曝光。两个10.3k×10.3k CCD，9微米像素，峰值量子效率为94- 96%，共记录92个中阶梯光栅阶数。我们介绍了一种新的变体的波导图像切片器与3，5，和7切片和峰值效率之间的92- 96%。共有六个交叉色散器覆盖摄谱仪的六个波长设置，其中两个总是同时进行。这些是由一个VPH光栅夹在两个棱镜。包括望远镜在内的系统的峰值效率在650 nm处为15%，在390 nm和900 nm处仍分别为11%和10%。结合LBT的110 m2光收集能力，我们预计在低分辨率模式下的极限星等为2000等（V）。R = 120 000模式也可以与两个双光束斯托克斯IQUV偏振计一起使用。270 000模式是通过7层图像切片器和100微米光纤通过0.74“的投影天空孔径实现的，与LBT站点的中值可视度相当。每分辨率元素12像素采样的43000模式是我们的视觉差或模糊对象模式。三种分辨率模式中的任何一种都可以与天空光纤一起使用，以实现同时的天空曝光，或者与来自稳定的法布里-珀罗标准具的光一起使用，以实现超精确的径向速度。CCD图像处理使用专用的数据简化和分析软件包PEPSI-S4 S进行。它的全部误差传播通过所有的图像处理步骤允许通过使用统计推断和鲁棒估计器的参数的自适应选择。一个太阳能饲料利用PEPSI在白天的时间和500米饲料从1.8米的VATT可以使用时，LBT是忙碌，否则。在本文中，我们提出了基本的仪器设计，它的实现，它的特点。一些预调试第一光光谱应证明基本功能。（© 2015 WILEY-VCH Verlag GmbH & Co. KGaA，魏因海姆）
PEPSI is the bench-mounted, two-arm, fibre-fed and stabilized Potsdam Echelle Polarimetric and Spectroscopic Instrument for the 2×8.4 m Large Binocular Telescope (LBT). Three spectral resolutions of either 43 000, 120 000 or 270 000 can cover the entire optical/red wavelength range from 383 to 907 nm in three exposures. Two 10.3k×10.3k CCDs with 9-µm pixels and peak quantum efficiencies of 94–96 % record a total of 92 echelle orders. We introduce a new variant of a wave-guide image slicer with 3, 5, and 7 slices and peak efficiencies between 92–96 %. A total of six cross dispersers cover the six wavelength settings of the spectrograph, two of them always simultaneously. These are made of a VPH-grating sandwiched by two prisms. The peak efficiency of the system, including the telescope, is 15 % at 650 nm, and still 11 % and 10 % at 390 nm and 900 nm, respectively. In combination with the 110 m2 light-collecting capability of the LBT, we expect a limiting magnitude of ≈20th mag in V in the low-resolution mode. The R = 120 000 mode can also be used with two, dual-beam Stokes IQUV polarimeters. The 270 000-mode is made possible with the 7-slice image slicer and a 100-µm fibre through a projected sky aperture of 0.74″, comparable to the median seeing of the LBT site. The 43 000-mode with 12-pixel sampling per resolution element is our bad seeing or faint-object mode. Any of the three resolution modes can either be used with sky fibers for simultaneous sky exposures or with light from a stabilized Fabry-Perot etalon for ultra-precise radial velocities. CCD-image processing is performed with the dedicated data-reduction and analysis package PEPSI-S4S. Its full error propagation through all image-processing steps allows an adaptive selection of parameters by using statistical inferences and robust estimators. A solar feed makes use of PEPSI during day time and a 500-m feed from the 1.8 m VATT can be used when the LBT is busy otherwise. In this paper, we present the basic instrument design, its realization, and its characteristics. Some pre-commissioning first-light spectra shall demonstrate the basic functionality. (© 2015 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)