Design and development of WFOS, the Wide-Field Optical Spectrograph for the Thirty Meter Telescope
Design and development of WFOS, the Wide-Field Optical Spectrograph for the Thirty Meter Telescope
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三十米望远镜宽视场光谱仪WFOS的设计与研制
DOI：
10.1117/12.2629464
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发表时间：
2022
期刊：
影响因子：
--
通讯作者：
Varshney, Hari Mohan
中科院分区：
文献类型：
--
作者：
Steidel, Charles C.;Peng, Eric W.;Fucik, Jason R.;Nash, Reston;Kaye, Stephen;Jacoby, George H.;Delabre, Bernard;Sethuram, Ramya;Divakar, Devika;Varshney, Hari Mohan
我们介绍了WFOS的当前设计，这是一种宽视场紫外/光学（0.31-1.0µm）成像光谱仪，计划用于TMT国际天文台30 m望远镜的首光。WFOS优化了在整个光波带的高灵敏度，可在8 '的连续视场上对非常微弱的目标进行低至中等分辨率（R ~ 1500-5000）长缝和多缝光谱分析。3×3”。在TMT的f/15内斯密斯焦点处。WFOS的一个关键设计目标是在所有观测模式下的稳定性和可重复性，这是通过其重力不变的光机械结构实现的，该结构具有垂直旋转轴，所有可重构组件仅在平行于Nasmyth平台的分层光学平台定义的平面上移动。WFOS的光学系统包括一个校正9 '直径场的线性ADC，包括科学FoV和4巡逻采集、引导和波前传感相机系统；一种新型的2镜反射准直器，使科学视场集中在望远镜光轴上；二向色分光器将准直光束分为2个波长优化的分光通道（蓝色：0.31-0.56µm，红色：0.54-1.04µm）；可选择的透射分散器（VPH和/或VBG）具有远程配置光栅倾斜（入射角）和相机衔接，能够优化衍射效率和波长覆盖在每个通道；全折射，波长优化的f/2光谱仪相机，以及UV/蓝色和红色优化的探测器系统。在从ADC到检测器的整个0.31-1µm范围内，WFOS对光谱的预测仪器通放平均为bbb56 %。当与30米TMT口径相结合时，WFOS将实现比目前8-10米级望远镜的灵敏度提高约20倍。
We present the current design of WFOS, a wide-field UV/optical (0.31-1.0 µm) imaging spectrograph planned for first-light on the TMT International Observatory 30 m telescope. WFOS is optimized for high sensitivity across the entire optical waveband for low-to-moderate resolution (R ∼ 1500-5000) long-slit and multi-slit spectroscopy of very faint targets over a contiguous field of view of 8′ .3×3 ′ .0 at the f/15 Nasmyth focus of TMT. A key design goal for WFOS is stability and repeatability in all observing modes, made possible by its gravity-invariant opto-mechanical structure, with a vertical rotation axis and all reconfigurable components moving only in planes defined by tiered optical benches parallel to the Nasmyth platform. WFOS’s optics include a linear ADC correcting a 9′ diameter field, including both the science FoV and 4 patrolling acquisition, guiding, and wavefront sensing camera systems; a novel 2-mirror reflective collimator allowing the science FoV to be centered on the telescope optical axis; a dichroic beamsplitter dividing the collimated beam into 2 wavelength-optimized spectrometer channels (blue: 0.31-0.56 µm; red: 0.54-1.04 µm); selectable transmissive dispersers (VPH and/or VBG) with remotely configurable grating tilt (angle of incidence) and camera articulation that enable optimization of diffraction efficiency and wavelength coverage in each channel; all-refractive, wavelength-optimized f/2 spectrograph cameras, and UV/blue and red-optimized detector systems. The predicted instrumental through put of WFOS for spectroscopy averages > 56% over the full 0.31-1 µm range, from the ADC to the detector. When combined with the 30 m TMT aperture, WFOS will realize a factor of ∼20 gain in sensitivity compared to the current state of the art on 8-10 m-class telescopes.
影响因子：
1.9
作者：
R. Buchroeder
通讯作者：
R. Buchroeder
Keck-I 卡塞格伦 ADC
DOI：
--
发表时间：
2008
期刊：
Astronomical Telescopes + Instrumentation
影响因子：
--
作者：
A. Phillips;Joseph S. Miller;D. Cowley;V. Wallace
通讯作者：
V. Wallace