dc.contributor.author |
Steidel, Charles |
|
dc.contributor.author |
Peng, Eric |
|
dc.contributor.author |
Fucik, Jason |
|
dc.contributor.author |
Nash, Reston |
|
dc.contributor.author |
Kaye, Stephen |
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dc.contributor.author |
Jacoby, George |
|
dc.contributor.author |
Delabre, Bernard |
|
dc.contributor.author |
Ramya, S |
|
dc.contributor.author |
Divakar, Devika |
|
dc.contributor.author |
Varshney, Hari Mohan |
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dc.contributor.author |
Sivarani, T |
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dc.contributor.author |
Uraguchi, Fumihiro |
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dc.contributor.author |
Ozaki, Shinobu |
|
dc.contributor.author |
Ji, Hangxin |
|
dc.contributor.author |
Tao, L V |
|
dc.contributor.author |
Chiu, Kent |
|
dc.contributor.author |
Zhu, Qinfeng |
|
dc.contributor.author |
Andersen, David |
|
dc.contributor.author |
Miles, John |
|
dc.contributor.author |
Lasi, Davide |
|
dc.date.accessioned |
2022-10-19T08:31:08Z |
|
dc.date.available |
2022-10-19T08:31:08Z |
|
dc.date.issued |
2022-08 |
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dc.identifier.citation |
Proceedings of the SPIE, Vol. 12184, pp.1218423-1- 1218423-14 |
en_US |
dc.identifier.issn |
1996-756X |
|
dc.identifier.uri |
http://hdl.handle.net/2248/8058 |
|
dc.description |
Restricted Access |
en_US |
dc.description.abstract |
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. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
SPIE-The International Society for Optical Engineering |
en_US |
dc.relation.uri |
https://doi.org/10.1117/12.2629464 |
|
dc.rights |
© SPIE-The International Society for Optical Engineering |
|
dc.subject |
Instrumentation |
en_US |
dc.subject |
Spectrograph |
en_US |
dc.subject |
TMT |
en_US |
dc.subject |
UV/optical |
en_US |
dc.subject |
Multi-slit spectrometer |
en_US |
dc.title |
Design and development of WFOS, the Wide-Field Optical Spectrograph for the Thirty Meter Telescope |
en_US |
dc.type |
Article |
en_US |