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Overview of Instrumentation at ING


This page gives an overview of the instrumentation available 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.

Notes (§) about specific instruments and procedures can be found at the bottom of the page.

Information about applying for telescope time can be found on a separate page.

In semester 2016B begins a series of changes at the WHT and INT, in preparation for the deployment of new survey instruments on both telescopes. AF2 and INTEGRAL will not be offered after semester 2016B.

The adaptive-optics instruments (NAOMI/INGRID, NAOMI/OASIS) are no longer offered, as a result of ongoing rationalisation of the instrumentation suite (and following a 2014 poll of the community).

Information about instruments no longer offered at ING can be found on a separate page.



Spectroscopy
Instrument/Contacts Wavelength
range
Resolving
power (§8)
Slit length Detector (§6) Comments
4.2-m William Herschel Telescope
Manager: Benn
ISIS
Specialist: Skillen / Hrudkova
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)
Specialist: Karjalainen / Fariña
9000 - 24000 Å 1000 < R < 3000 4.2' HgCdTe Long-slit spectroscopy;
multi-object spectroscopy;
spectro and imaging polarimetry
ACAM (§2)
Specialist: Benn / Domínguez  
3500 - 9400 Å R ~ 400 6' AUXCAM Long-slit spectroscopy
AF2/WYFFOS (§3)
Specialist: Domínguez / Fariña
3500 - 10000 Å 100 < R < 3000
(reflection mode)
R = 9500
(echelle mode)
1.6" fibres Red+4 (or WHTWFC) Up to 150 objects
2.5-m Isaac Newton Telescope
Manager: Fariña
IDS
Specialist: Fariña / Domínguez
3000 - 10000 Å 700 < R < 10000 3.3' Red+2 (or EEV10)
Long-slit spectroscopy


Imaging
Instrument/Contacts Detector (§6) Filters (§7) Scale ("/pixel) Field-of-view
4.2-m William Herschel Telescope
Manager: Benn
Prime-Focus Camera
Specialist: Vaduvescu / Benn
WHTWFC See database 0.24 18' x 18'
(Red+4)
ACAM (§2)
Specialist: Benn / Domínguez  
AUXCAM Most ING filters, see database 0.25 8'.3
LIRIS
Specialist: Karjalainen / Fariña
HgCdTe ZJHK_s
and 8 narrow-band
0.25 4'.27
2.5-m Isaac Newton Telescope
Manager: Fariña
Wide Field Camera (§4)
Specialist: Vaduvescu / Hrudkova
EEV See database 0.33 33'.8 x 33'.8


Visitor Instruments (§5)
InstrumentDescription Institute Contact
4.2-m William Herschel Telescope
Manager: Benn
GHaFaS Fabry-Perot Hα imager IAC John Beckman
INTEGRAL Fibre-bundle integral-field spectrograph IAC Evencio Mediavilla
PAUCam(§9) Prime-focus imager 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

  1. LIRIS: slit-mask preparation and manufacture takes approximately eleven weeks; PIs awarded time in multi-slit mode are strongly encouraged to initiate the design of slit masks at the earliest opportunity. Information about slit-mask design and timelines is given here. As of semester 2014B, the cost of manufacturing the slit masks (600 - 900 euros per mask) must be covered by the home institution of the proposing team.
  2. ACAM: observations can be made at any time, except when an instrument is mounted at WHT prime focus.
  3. AF2: improvements to the target-acquisition procedure and to the mapping of field distortion at WHT prime focus have improved the acquisition accuracy to better than 0.4 arcsec for 90% of fibres out to 20 arcmin from the center of the field of view (beyond this radius, there is significant vignetting). For reference, in seeing of 0.5 - 1.5 arcsec, a fibre-centring error of 0.4 arcsec leads to ~ 10% loss of light from a point source, relative to that from a well-centred fibre. Teams applying to use AF2 are encouraged to check the latest AF2 news.
  4. INT WFC: offered at rotator angle 180 degrees only. When there is compelling scientific justification, other rotator angles (0, 90 or 270-degrees) can be offered for the duration of the run; changes to the rotator angle within a run are not permitted.
  5. Visitor instruments: applicants wishing to submit proposals to use these should in the first instance contact the relevant person named in the above table. Applicants wishing to submit a proposal based on a new (to ING) visitor instrument should follow these instructions. After 2016B, visiting instruments requiring a Nasmyth focus will be hosted on the GRACE Nasmyth platform (rather than GHRIL).
  6. CCDs: specifications and technical details are given on the ING detectors page.
  7. Filters: details are given on the ING filters page.
  8. Spectroscopic resolutions quoted for ISIS, LIRIS, ACAM and IDS assume a 1-arcsec slit.
  9. The PAUCam team are making their instrument available to the ING community in 2016B at the observers' risk. Commissioning results are being posted at the PAUCam web pages as they become available. The autoguiding functionality will probably be commissioned in 2016A and may be available in 2016B. Observers interested in using PAUCam in 2016B should contact Francisco Castander at the email address above, for the latest advice about any performance issues not addressed in the PAUCam web pages, and also for advice about the likely timing of PAUCam survey runs during 2016B. All scheduled observations will be carried out by the PAUCam team.


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Contact:  (Head of Astronomy)
Last modified: 19 February 2016