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Home > Astronomy > Overview of Instrumentation |
Overview of Instrumentation at INGThis page provides an overview of the instrumentation at the WHT and INT. Further information about a given instrument can be obtained by clicking on the instrument name, or by emailing one of the listed instrument specialists. At the INT, the usual instruments (IDS, WFC) are offered in 2021B. At the WHT, it is expected that commissioning and science verification of the new multi-object spectrograph WEAVE will begin in June 2021, and the WEAVE science surveys should start a few months later. From then on, a long-term average of 70% of the time at the WHT will be devoted to the WEAVE surveys. The remaining 30% of the time will be available for 'open time' community observing with the current Cassegrain instruments (ISIS, LIRIS, ACAM) or with visiting instruments, or with WEAVE itself. Open time will not be advertised until WEAVE is commissioned. Because of instrument-change overheads, WEAVE will probably be mounted on the telescope for periods ~ 9 months at a time. On current plans, the first such period of observing with WEAVE will not end before early-2022. The latest news about the ongoing evolution of the instrumentation at the WHT and INT (following a 2014 poll of the community) can be found on the ING instrumentation update page. Information about how to apply for telescope time can be found on the applying for telescope time page. Notes (§) about specific instruments and procedures can be found at the bottom of this page. Information about instruments no longer offered at ING (e.g. the multi-object spectrograph AF2) can be found on the page about past, present and future instruments. |
Spectroscopy | |||||
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Instrument/Contacts | Wavelength range |
Resolving power (§7) |
Slit length | Detector (§5) | Comments |
4.2-m William Herschel Telescope
Manager: Benn |
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ISIS
Specialists: Skillen / Benn |
3000 - 10000 Å | 600 < R < 12700 | 4' | Red:
Red+ Blue: EEV12 Red or Blue: Qucam3, Qucam2 |
Long-slit spectroscopy; spectro and imaging polarimetry; fast spectroscopy; image-slicer |
LIRIS (§1)
Specialists: Dominguez / Fariña |
9000 - 24000 Å | 1000 < R < 3000 | 4.2' | HgCdTe | Long-slit spectroscopy; multi-object spectroscopy; spectro and imaging polarimetry |
ACAM (§2)
Specialists: Benn / Domínguez |
3500 - 9400 Å | R ~ 400 | 6' | AUXCAM | Long-slit spectroscopy |
WEAVE (to be commissioned in 2020)
Specialists: Benn / Domínguez / Fariña |
3660 - 9590 Å | R ~ 5000, 20000 | EEV CCDs | MOS (up to 960 fibres) and IFU spectroscopy | |
2.5-m Isaac Newton Telescope
Manager: Fariña |
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IDS
Specialists: Domínguez / Fariña |
3000 - 10000 Å | 700 < R < 10000 | 3.3' |
Red+2
(or
EEV10) |
Long-slit spectroscopy |
Imaging | |||||
---|---|---|---|---|---|
Instrument/Contacts | Detector (§5) | Filters (§6) | Scale ("/pixel) | Field-of-view | |
4.2-m William Herschel Telescope
Manager: Benn |
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ACAM (§2)
Specialists: Benn / Domínguez |
AUXCAM | Most ING filters, see database | 0.25 | 8'.3 | |
LIRIS
Specialists: Dominguez / Fariña |
HgCdTe | ZJHK_s and 8 narrow-band |
0.25 | 4'.27 | |
2.5-m Isaac Newton Telescope
Manager: Fariña |
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Wide Field Camera (§3) Specialists: Vaduvescu / |
EEV | See database | 0.33 | 33'.8 x 33'.8 |
Visitor Instruments (§4) | |||
---|---|---|---|
Instrument | Description | Institute | Contact |
4.2-m William Herschel Telescope
Manager: Benn |
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GHaFaS | Fabry-Perot Hα imager | IAC | John Beckman, Alex Oscoz |
PAUCam(§8) | Prime-focus imager (1 deg field of view) | IFAE | Francisco Castander |
PN.S | Slitless counter-dispersed spectrograph | Kapteyn | Magda Arnaboldi |
SIGNAL can
be used to calculate exposure times for most
telescope/instrument/detector combinations.
§ Notes
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