Optical/infrared telescopes available to UK astronomers (2010 September)


 

This is a list and basic details of the ground-based optical and infrared observing facilities which accept applications for telescope time from UK astronomers. The list is sorted according to observing type and wavelength domain, and includes basic details on each instrument (resolution, field size, etc). All information on this page is supplied without guarantee of correctness.

This webpage does not include some of the OPTICON telescopes at present.

 


WHT     --     INT     --     NOT     --     TNG     --     LT     --     GTC     --     CAHA     3.5m     2.2m     1.2m     --     UKIRT     --     Gemini     North     South     --     KPNO    
ESO Paranal     VLT     --     VISTA     ESO La Silla     3.6m     NTT     2.2m     --     LCO     Baade     Clay     2.5m     1.0m        
CTIO     4.0m     SOAR     1.5m     1.3m     1.0m     0.9m     --     SAAO     SALT     1.9m     1.0m     --     AAT    


Overview of capabilities


Optical imaging

Optical spectroscopy

Optical échelle spectroscopy

Infrared imaging

Infrared spectroscopy

Infrared échelle spectroscopy


Optical wavelengths Infrared wavelengths

Imaging Spectroscopy Échelle spec. Imaging Spectroscopy Échelle spec.
 
 
      La Palma   (Spain)
  WHT 4.2m PFIP   ACAM ISIS   WYFFOS
OASIS   ACAM

INGRID   LIRIS LIRIS
  INT 2.5m WFC IDS



  NOT 2.5m ALFOSC   MOSCA   StanCam ALFOSC FIES NOTCAM
NOTCAM

  TNG 3.6m DOLORES   OIC DOLORES SARG NICS NICS
  LT 2.0m RATCam   RISE FRODOspec



  GTC 10.4m OSIRIS OSIRIS
CanariCam CanariCam
 
 
      Calar Alto   (Spain)
  3.5m LAICA   MOSCA MOSCA   PMAS   TWIN
Omega-2000
Omega-Cass


  2.2m BUSCA   CAFOS   AstraLux CAFOS
MAGIC MAGIC
  1.2m CCD




 
 
      UK Infrared Telescope   (Hawaii)
  3.8m UKIRT


WFCAM

 
 
      Gemini   (Hawaii and Chile)
  Gemini North GMOS GMOS
NIRI   MICHELLE NIRI   NIFS   MICHELLE
  Gemini South GMOS GMOS
T-ReCS T-ReCS
 
 
      European Southern Observatory   (Paranal, Chile)
  VLT UT1 FORS2 FORS2


CRIRES
  VLT UT2 FORS1
FLAMES / GIRAFFE
UVES
FLAMES / UVES
X-SHOOTER


X-SHOOTER
  VLT UT3 VIMOS VIMOS
VISIR / ISAAC VISIR / ISAAC
  VLT UT4


NACO   HAWK-I NACO   SINFONI
  VISTA


OmegaCAM

 
 
      European Southern Observatory   (La Silla, Chile)
  3.6m

HARPS


  NTT 3.6m EFOSC EFOSC
SofI SofI
  2.2m MPI WFI
FEROS


 
 
      Las Campanas Observatory   (Chile)
  Magellan Baade IMACS IMACS
PANIC FIRE
  Magellan Clay MagIC MagE MIKE


  2.5m du Pont CCD   WFCCD B & C Échelle WIRC

  1.0m Swope CCD

RETROCAM

 
 
      Kitt Peak National Observatory   (Arizona, USA)
  4m Mayall MOSAIC R-C   MARS Échelle NEWFIRM   SQIID  FLAMINGOS FLAMINGOS   IRMOS
  2.1m CCD GoldCam
SQIID  FLAMINGOS FLAMINGOS
  WIYN 3.5m MIMO   OPTIC Hydra
WHIRC

  WIYN 0.9m MOSAIC




 
 
      Cerro Tololo Inter-American Observatory   (Chile)
  4m Blanco MOSAIC-II R-C   HYDRA
ISPI

  4.1m SOAR SOI   HTS HTS
OSIRIS OSIRIS
  1.5m
R-C
CPAPIR

  1.3m ANDICAM

ANDICAM

  1.0m Y4KCAM




  0.9m CCD




 
 
      South African Astronomical Observatory
  SALT SALTICAM




  1.9m Radcliffe CCD camera   UCT CCD GratingSpec GIRAFFE


  1.0m CCD camera   UCT CCD




 
 
      Anglo-Australian Observatory   (Siding Springs, Australia)
  4.0m AAT
AAOmega UCLES   UHRF IRIS2 IRIS2
 

Imaging Spectroscopy Échelle spec. Imaging Spectroscopy Échelle spec.

Optical wavelengths Infrared wavelengths

 


Telescope availability and applying for time

Many of the application deadlines are general guidelines only, based on experience from previous years. Anyone wishing to submit an application should confirm these dates (and all other relevant information in this document) directly on the official webpages of the telescope concerned. You have been warned.....

Telescopes Deadlines Semesters Notes
  WHT
 
INT
~15 September
~15 March
1 February to 31 July
1 August to 31 January
UK astronomers have ~40% share (but decreasing) on these telescopes.
  UKIRT ~15 August
~15 March
1 February to 31 July
1 August to 31 January
UKIRT is now run in campaign mode, but a small proportion of its time is available for applciations in the usual way through PATT. The UK now conducting a phased withdrawal from UKIRT. There may be no more calls for proposals.
  ESO ~31 March
~30 September
1 October to 31 March
1 April to 30 September
The UK is a member of ESO so can apply for all ESO telescopes.
  Gemini ~2 April
~30 September
1 August to 31 January
1 February to 31 July
The UK is (currently) a member of Gemini with full access to the telescopes. This situation is not expected to last for a long time.
  LT ~15 September
~15 March
1 February to 31 July
1 August to 31 January
UK astronomers have a share on this telescope through PATT.
  AAT ~1 September
~1 March
1 February to 31 July
1 August to 31 January
UK astronomers can apply via OPTICON.
  NOT ~1 September
~1 March
1 October to 31 March
1 April to 31 September
UK astronomers can apply via OPTICON.
  TNG ~1 September
~1 March
1 August to 31 January
1 February to 30 July
UK astronomers can apply via OPTICON.
  Calar Alto ~1 September
~1 March
1 July to 31 December
1 Jan to 30 June
UK astronomers can apply via OPTICON.
  LCO

Available only through Carnegie, a few other US institutions, or Chilean time.
  CTIO 31 March
30 September
August to January
February to July
Available through NOAO. Non-US astronomers must justify why they need to use US facilities (i.e. why they cannot use other facilities which are available to them).
  KPNO 31 March
30 September
August to January
February to July
Available through NOAO. Non-US astronomers must justify why they need to use US facilities (i.e. why they cannot use other facilities which are available to them).
  SAAO 1 October
18 December
1 April
1 July
January to March
April to June
July to September
October to December
A "certain percentage" of time goes to astronomers of any nationality. This may not apply to SALT, which is restricted to the members of the SALT consortium.
  GTC ~31 March
~30 September
Large programs only (10+ nights) The GTC was for a while available through ESO, but no new applications will be accepted.

OPTICON also grants access to the Carlos Sanchez telescope (Tenerife), the 1.9m OHP telescope (Provence), the TBL 2m telescope (Pyrenees) and the CFHT 3.6m (Hawaii).

 


Basic details of telescopes and instruments

 


Optical imaging

Optical spectroscopy

Optical échelle spectroscopy

Infrared imaging

Infrared spectroscopy

Infrared échelle spectroscopy

La Palma

Isaac Newton Group (ING)

4.2m William Herschel Telescope (WHT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
ISIS Long-slit spectroscopy Blue: 3500 to 5100 Å
Red: 5400 to 10000 Å
Blue: 0.11 to 1.62 Å/px
Red: 0.26 to 1.81 Å/px
Blue: EEV 4k × 2k CCD
Red: REDPLUS 4k × 2k
Either arm: an L3CCD with almost zero readout noise is available.
3.7 arcmin slit length It has a dichroic, and does observations in the blue and red arms simultaneously
WYFFOS Multi-object spectroscopy 3700 to 10000 Å 0.06 to 2.9 Å/px Mosaic of two EEV 4k × 2k CCDs 20 arcmin unvignetted Uses ISIS gratings (or échelle). Up to 150 fibres available.
NAOMI/OASIS Integral-field spectroscopy 4200 to 9900 Å 0.37 to 35 Å/px MIT/LL3 4k × 2k CCD 3.7 × 2.7 arcsec to 10.3 × 7.4 arcsec Has 1100 lenslets. Can use the NAOMI adaptive optics system. Used to be at the CFHT.
PFIP Wide-ish field imaging U B V R I Z
(other filters available)
0.24 arcsec/px Mosaic of two EEV 4k × 2k CCDs 16.2 × 16.2 arcmin Prime focus imaging camera
ACAM Optical imaging U B V R I Z plus narrow-band filters 0.25 arcsec/px AUXCAM (2048 × 4096 EEV CCD) circular, 8.3 arcmin in diameter Always mounted except for when the PFIP is in use, so is good for over-rides and ToOs.
ACAM Low-resolution spectroscopy 3500 to 9000 Å R ~ 250-900 depending on slit and wavelength AUXCAM (2048 × 4096 EEV CCD) 5.8 arcmin long slit Always mounted except for when the PFIP is in use, so is good for over-rides and ToOs.
NAOMI/INGRID High-resolution IR imaging 0.8 to 2.5 micron 0.04 arcsec/px HgCdTe 1k × 1k array 40 × 40 arcsec Uses the NAOMI adaptive optics system
LIRIS IR imaging 0.8 to 2.5 micron 0.25 arcsec/px HgCdTe 1k × 1k array 4.27 × 4.27 arcmin
LIRIS Low-resolution IR spectroscopy 0.8 to 2.5 micron R = 700 to 2500 HgCdTe 1k × 1k array long slits available

The long-term future of the WHT is not completely secure as its present status is reliant on funding from several Governments, one of which (UK) is becoming increasingly reticent. However, the WHT is an excellent telescope which is also demonstrably cheap to run. It is being steered towards wide-field multi-object spectroscopy, in which case it will be a good survey instrument to support the larger northern telescopes.

2.5m Isaac Newton Telescope (INT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
IDS Long-slit spectroscopy 3500 to 9000 Å 0.24 to 3.7 Å/px EEV 4k × 2k CCD 3.3 arcmin slit width The 235mm camera is available.
The 500mm camera (higher dispersion) is not offered.
WFC Wide field imaging 3500 to 9000 Å
(many filters available)
0.33 arcsec/px Mosaic of four EEV 4k × 2k CCDs 34.2 × 34.2 arcmin (in an L shape) Readout time 40s. Binning and windowing has apparently been implemented recently (2011A AO).

The future of the INT is not secure, and depends on the ING being given sufficient funding for its continued low-level operation. At present (2010) the UK government is actively seeking to minise the funding it give to the ING, which is not a good sign for the INT. The telescope is productive but coming towards the end of its economic lifetime.

2.5m Nordic Optical Telescope (NOT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
ALFOSC Grism spectroscopy 3200 to 11000 Å R = 190 to 10000 EEV 2k × 2k Roughly 5 arcmin Also has a multi-object spectroscopy mode. Readout time 90s (unbinned) or 32s (2×2). Also does polarimetry.
ALFOSC Optical imaging 3200 to 9100 Å 0.19 arcsec/px EEV 2k × 2k 5 to 7 arcmin depending on the filter Also does polarimetry.
MOSCA
Mosaic Camera
Optical imaging UBVRI ugriz uvbyβ 0.11 arcsec/px Mosaic of four Loral 2k × 2k CCDs 7.7 × 7.7 arcmin Readout time 113s (unbinned) or 37s (2×2 binning).
StanCam Optical imaging U B V R I 0.176 arcsec/px TEK 1k × 1k CCD 3 × 3 arcmin Permanently mounted. Also used as slit viewer for FIES. Readout time 43s (unbinned) or 16s (2×2).
NOTCAM IR imaging 0.8 to 2.5 micron 0.23 or 0.08 arcsec/px HgCdTe 1k × 1k array 4×4 arcmin or 82×82 arcsec Also does polarimetry.
NOTCAM IR grism spectroscopy 0.8 to 2.5 micron R = 2500 or 5500 HgCdTe 1k × 1k array Slit length 4 arcmin or 80 arcsec
FIES Optical échelle spectroscopy 4000 to 8300 Å R = 25 000, 45 000 or 65 000 EEV 2k × 2k CCD Poor response in the blue due to long fibres. Can do a simultaneous thorium-argon wavelength calibration mode.

The short-term future of the NOT is stable as the Nordic countries are fully aware of its high capability, reliability and low running costs. The FIES spectrograph is excellent. In the longer term there are indications that it may struggle to attract a high number of applications for observing time, although it would be a valued part of the prospective Common Northern Observatory.

3.6m Telescopio Nazionale Galileo (TNG)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
SARG Optical échelle spectroscopy 3700 to 10000 Å R = 29 000 to 164 000 Mosaic of two EEV 4k × 2k CCDs Long-slit observations can cover up to 30 arcsec
NICS IR imaging 0.9 to 2.5 micron 0.25 to 0.04 arcsec/px HgCdTe 1k × 1k array 4.2×4.2 to 0.7×0.7 arcmin Has two different cameras. Can do polarimetry.
NICS IR grism spectroscopy 0.9 to 2.5 micron 2 to 100 Å/px HgCdTe 1k × 1k array Can do spectropolarimetry.
LRS / DOLORES Optical imaging UBVRI and ugriz
plus additional filters
0.275 arcsec/px Loral 2k × 2k CCD 9.4 × 9.4 arcmin Readout time 20s (unbinned) or 6s (2×2 binning).
LRS / DOLORES Optical low-resolution spectroscopy 3700 to 10000 Å R = 300 to 5000 Loral 2k × 2k CCD 9.4 arcmin field for MOS. Can do multi-object spectroscopy. Readout time 20s (unbinned) or 6s (2×2 binning) for full CCD.
OIG Optical imaging UBVRI and ugriz
plus additional filters
0.072 arcsec/px Mosaic of two EEV 4k × 2k CCDs 4.9 × 4.9 arcmin Readout time 216s (unbinned) or 66s (2×2) or 37s (3×3).

The future of the TNG must be regarded as uncertain as it is desperately short of money. However, it is expected to benefit from hosting the HARPS-NEF spectrograph, which is intended for follow-up of transiting planet candidates discovered by the Kepler satellite.

2.0m robotic Liverpool Telescope (LT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
RATCam Optical imaging ugriz and BV and Hα 0.135 arcsec/px EEV 2k × 2k CCDs 4.6 × 4.6 arcmin Readout time 10s (unbinned) or 5s (2×2). 3×3 and 4×4 binning also available.
RISE Optical high-speed imaging V+R filer (roughly 4600 to 7200 Å) 0.54 arcsec/px EEV frame-transfer CCD 9.2 × 9.2 arcmin Readout speed is "less than a second".
FRODOspec Optical medium-resolution spectroscopy 3900 to 9400 Å R = 2200 to 5500 CCDs 11 × 11 arcsec Integral-field spectrograph. Has a red and a blue arm which and are capable of obtaining the full optical/near-IR wavelength region in one observation.

There is also the Meanburn spectrograph but this is not a common-user instrument. The future of the telescope is uncertain at this point due to funding difficulties.

10.4m Gran Telescopio Canarias (GTC)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
OSIRIS Optical imaging 3650 to 10500 Å with ugriz plus tunable filters 0.125 arcsec/px Mosaic of two MIT/LL 2k × 2k CCDs 8.53 × 8.67 arcmin Can do long-slit and multi-object spectroscopy too
OSIRIS Optical spectroscopy 3650 to 10500 Å R = 325 to 2500 Mosaic of two MIT/LL 2k × 2k CCDs 8 × 5 arcmin Can do multi-object spectroscopy (up to 30 targets at once)
CanariCam Mid-IR imaging 8 to 25 microns 0.08 arcsec/px 320 × 240 pixel Si:As Raytheon 25.6 × 19.2 arcsec Can do coronography too
CanariCam Mid-IR spectroscopy 8 to 25 microns R = 175 to 1310 320 × 240 pixel Si:As Raytheon 19.2 arcsec long slit Can do polarimetry too

 


Calar Alto

3.5m telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
LAICA Wide-field optical imaging 3400 to 10000 Å 0.225 arcsec/px Mosaic of four 4k × 4k CCDs 44.36 × 44.36 arcmin (requires four observations) CCDs are separated by just under one CCD width in each direction, so four observations are needed to fully cover one field.
TWIN Optical spectroscopy blue: 3500 to 5000 Å
red: 5000 to 10000 Å
0.36 to 2.2 Å/px Two SITe 2048×800 CCDs Slit length up to 4 arcmin Blue and red arms can operate simultaneously
MOSCA Optical imaging 3300 to 10000 Å 0.33 arcsec/px Normally uses one 4k × 2k CCD 11 × 11 arcmin Also does grism and multi-object spectroscopy.
MOSCA Optical grism spectroscopy with MOS capability 3300 to 10000 Å 1 to 4 Å resolution Normally uses one 4k × 2k CCD 11 × 11 arcmin Also does imaging and multi-object spectroscopy.
OMEGA-2000 Wide-field IR imaging zJHK 0.45 arcsec/px HgCdTe 2k × 2k array 15.4 × 15.4 arcmin Mounted at prime focus.
OMEGA-Cass IR adaptive-optics imaging zJHK 0.3 to 0.04 arcsec/px HgCdTe 2k × 2k array 5×5 arcmin to 40×40 arcsec Mounted at Cassegrain focus and uses the ALFA laser-guided adaptive optics. Also does polarimetry and spectroscopy.
PMAS Optical integral-field spectroscopy 3500 to 9000 Å resolution is 0.5 to 2.7 arcsec; dispersion is 0.35 to 1.7 Å/px 4k × 2k CCD, but a 4k × 4k mosiac is under construction 8×8 to 74×65 arcsec

Omega-Cass is currently only available for imaging.

2.2m telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
BUSCA Optical imaging (simultaneous in four bands) Optical wavelengths 0.176 arcsec/px Four 4k × 4k CCDs (the bluemost one thinned) 12 × 12 arcmin Dichroics split the light beam with cut-off wavelengths around 4300, 5300 and 7000 Å. Readout time is large (about 2min).
AstraLux Optical "lucky" imaging 400 to 900 nm 0.044 arcsec/px 512 × 512 pixel electron-multiplying CCD 23 × 23 arcsec !!! Can run faster than 100 Hz with windowing
CAFOS Optical imaging 320 to 1100 nm EEV: 0.53 arcsec/px
Loral: 0.33 arcsec/px
Choice of two 2k × 2k CCDs: EEV (blue-sensitive) or Loral (red-sensitive). EEV: 16 × 16 arcmin
Loral: 10.8 × 10.8 arcmin
Also does polarimetry and spectroscopy.
CAFOS Optical grism spectroscopy Optical wavelengths 2.0 to 9.8 Å/px Choice of two 2k × 2k CCDs: EEV (blue-sensitive) or Loral (red-sensitive). EEV: 16 × 16 arcmin
Loral: 10.8 × 10.8 arcmin
Also does imaging and spectropolarimetry and multi-object spectroscopy.
MAGIC IR imaging 1.0 to 2.5 microns
(JHK)
1.62 or 0.64 arcsec/px HgCdTe 256 × 256 pixel array 6.9×6.9 or 2.7×2.7 arcmin Also does grism spectroscopy
MAGIC IR grism spectroscopy 1.0 to 2.5 microns R = 260 with 2-pixel slit HgCdTe 256 × 256 pixel array Also does imaging

1.23m telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
CCD Optical imaging BVRI plus other CAHA filters 0.5 arcsec/px SITe2b 2k × 2k CCD 16 × 16 arcmin (BVRI)
11 × 11 arcmin (other CAHA filters)
Operated remotely. Applications may need to be for large projects requiring many nights.

The observatory also has a 0.8m Schmidt telescope which is no longer used, and a 1.5m telescope which is operated by a separate group and used only intermittently.

MAGIC is available only at the 2.2m at present, but may become available at the 3.5m and 1.23m as well.

 


3.8m United Kingdom Infrared Telescope (UKIRT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
WFCAM Infrared imaging 1 to 5 microns 0.40 arcsec/px Mosaic of four HgCgTe 2k × 2k arrays cover a quarter of a 53×53 arcmin field in one observation 40 × 40 arcmin Four pointing are needed to fully cover each 53×53 arcmin field.

UKIRT is now running in campaign mode: the UKIDSS survey is being completed as quickly as possible and only the WFCAM instrument is available. From the UKIRT webpage on 17/8/2010: At this time it is not clear whether a Call for Proposals will be issued for 11A. Please visit the UKIRT homepage in early September for an update.

 


European Southern Observatory (ESO)

Paranal observatory (VLT)

8.2m VLT Unit Telescope 1 (Antu)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
CRIRES IR échelle spectroscopy 0.94 to 5.4 microns R = 100 000 Mosaic of four InSb arrays giving total size 4096 × 512 pixels Slit length is 40 arcsec at 0.086 arcsec/px Can use the MACAO adaptive optics instrument
FORS2 Optical imaging Optical, but lowish blue sensitivity 0.25 or 0.125 arcsec/px Mosaic of two MIT (red-sensitive) or EEV (blue-sensitive) 2k × 4k CCDs 6.8 × 6.8 arcmin or 4.25 × 4.25 arcmin Now has the polarimetry module which was on FORS1.
FORS2 Optical grism spectroscopy Optical, but lowish blue sensitivity Å R = 260 to 2600 Mosaic of two MIT (red-sensitive) or EEV (blue-sensitive) 2k × 4k CCDs 6.8 × 6.8 arcmin Also does multi-object spectroscopy. Now has the polarimetry module and some grisms from FORS1.

8.2m VLT Unit Telescope 2 (Kueyen)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
FLAMES / GIRAFFE Optical multi-object and integral-field spectroscopy 3700 to 9500 Å R = 10 000 or 25 000 EEV 2k × 4k CCD Deployable IFU allows spectroscopy of 15 objects, each with 20 microlenses (totalling 2×3 arcsec).
ARGUS IFU allows spectroscopy of one object using 22×14 microlenses (6.6×4.2 or 11.5×7.3 arcsec).
MEDUSA fibres allow 132 spectra to be obtained in one exposure, covering the 25 arcmin field.
FLAMES / UVES Optical multi-object échelle spectroscopy Red optical wavelengths R = 47 000 See UVES entry (uses red arm only) Up to 8 fibres are available per exposure FLAMES feeds 6 or 8 fibres to the entrance slit of the UVES spectrograph.
UVES Optical échelle spectroscopy 3000 to 5000 (blue) and 4200 to 11 000 (red) Å R = 40 000 to 110 000 Blue arm: EEV 4k × 2k CCD
Red arm: Mosaic containing one EEV 4k × 2k CCD and one Loral 4k × 2k CCD
Long slit maximum is less than 10 arcsec to avoid different orders merging. Has a blue and a red arm, which can either operated separately or simultaneously using a dichroic.
X-SHOOTER Simultaneous optical-IR échelle spectroscopy 3000 to 5595 Å (blue)
5595 to 10240 Å (red)
10240 to 24800 Å (IR)
R = 4500 (blue/IR)
R = 7000 (red)
EEV 4k × 2k CCD (blue), 4k × 2k MIT/LL CCD (red), 2k × 1k Hawaii (IR) 12 arcsec long slit, plus the option of an image-slicer IFU to improve resolution. Covers the wavelength range 0.3 to 2.5 μm in ONE exposure using three arms. Optimised for throughput, with a total efficiency of 30% (instrument + telescope + atmosphere).

8.2m VLT Unit Telescope 3 (Melipal)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
VIMOS Optical wide-field imaging U B V R I z 0.205 arcsec/px Each arm has one EEV 4k × 2k CCD Four arms, each with field of view 7×8 arcmin Also does MOS and IFU spectroscopy.
VIMOS Optical MOS and IFU spectroscopy 3600 to 10000 Å R = 200 to 2500 Each arm has one EEV 4k × 2k CCD MOS: Four arms, each 7×8 arcmin
IFU: 13×13 to 54×54 arcsec.
Also does imaging. The IFU has 6400 fibres.
VISIR Mid-IR imaging 8 to 13 micron (N) and 16.5 to 24.5 micron (Q) N: 0.075 arcsec/px
Q: 0.127 arcsec/px
DRS 256 × 256 BIB detector N: 19.2 × 19.2 arcsec
Q: 32.3 × 32.3 arcsec
Also does spectroscopy.
VISIR Mid-IR spectroscopy 8 to 13 micron (N) and 16.5 to 24.5 micron (Q) R = 350 to 25 000 DRS 256 × 256 BIB detector Slit length 32.3 to 4.1 arcsec Also does imaging.
ISAAC IR imaging 1 to 5 microns 0.148 or 0.071 arcsec/px Choice of two 1k × 1k arrays: HgCdTe (1 to 2.6 micron) or InSb (3 to 5 micron and JHK imaging) 152×152 or 73×73 arcsec Expected to be decommissioned during 2011 in favour of SPHERE. Can use the MACAO adaptive optics instrument.
ISAAC IR grating spectroscopy 1 to 5 microns R = 500 to 1000 Choice of two 1k × 1k arrays: HgCdTe (1 to 2.6 micron) or InSb (3 to 5 micron and JHK imaging) Slit length 120 arcsec Can use the MACAO adaptive optics instrument

8.2m VLT Unit Telescope 4 (Yepun)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
SINFONI IR integral field spectroscopy 1.1 to 2.45 microns Spatial: 0.025 or 0.1 or 0.25 arcsec per image slice
Spectral: R = 1500 to 4000
2k × 2k Hawaii 2RG detector 8×8 or 3×3 or 0.8×0.8 arcsec Has adaptive optics.
NACO
(NAOS-CONICA)
IR imaging 1 to 5 microns 0.0133 to 0.0547 arcsec/px 1k × 1k Aladin InSb array 14×14 to 56×56 arcsec Requires the NAOS adaptive optics. Also does polarimetry. Expected to be decommissioned by the end of 2011 and replaced by MUSE.
NACO
(NAOS-CONICA)
IR grism spectroscopy 1 to 5 microns R = 400 to 1700 1k × 1k Aladin InSb array 14×14 to 56×56 arcsec Requires the NAOS adaptive optics. Also does polarimetry.
HAWK-I IR imaging 0.85 to 2.55 microns 0.1063 arcsec/px Mosaic of four Hawaii 2k × 2k detectors 7.5×7.5 arcmin

4m VISTA Visible and Infrared Survey Telescope for Astronomy

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
OmegaCAM Near-infrared wide-field imaging Z Y J H Ks 0.339 arcsec/px Mosaic of 16 2k×2k HgCdTe detectors 1.65 degress in diameter The CCDs are not butted together and require four pointings to cover the full field of view without gaps.

Other facilities at Paranal

The VLT also has a well-developed interferometric capibility, which can either use several of the Unit Telescopes or the dedicated 2m Auxiliary Telescopes. Details of these facilities can be found from the Paranal instruments page.

A 2.6m VLT Survey Telescope (VST) is nearing completion at Paranal and will be equipped with a wide-field optical camera which is a mosaic of 32 CCDs with a field of view of 1×1 degree.

La Silla Observatory

The future of La Silla Observatory is not assured in the long term, as ESO seeks to shift its funding (which is already focussed on the VLT) to ALMA and construction of an Extremely Large Telescope. There has been a shift towards minimising the number of instruments: the 3.6m has only HARPS and the NTT has only SofI and EFOSC. SofI will be kept running as long as it is technically expedient, so could potentially become ununsable at any time. La Silla will operate until at least 2012. Information on the retired instruments can be found here: SUSI-2, EMMI, TIMMI2 and CES.

Changes from P84 on: visiting astronomers will be assigned a support astronomer but the SA will remain in Santiago rather than being available at the telescopes. A visiting astronomer will still have a telescope operator to operate the telescope.

3.6m telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
HARPS Optical échelle spectroscopy 3780 to 6910 Å R = 120 000 (standard). Also has wider fibre for higher throughput and lower resolution. Two EEV 4k × 2k CCDs Fibre opening is 1 arcsec diameter. Probably the world's best spectrograph. Simultaneous thorium-argon mode allows wavelength stability of 0.5 m/s. Also does spectropolarimetry.

3.6m New Technology Telescope (NTT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
EFOSC Optical imaging 3500 to 11000 Å 0.13 arcsec/px Loral 2k × 2k CCD 4.4 × 4.4 arcmin Also does long-slit and multi-object spectroscopy and polarimetry.
EFOSC Optical grism spectroscopy 3200 to 11000 Å 0.92 to 6.66 Å/px
plus new VPH grisms with R = 4000
Loral 2k × 2k CCD 4.4 × 4.4 arcmin Also does imaging and multi-object spectroscopy and polarimetry.
SofI IR imaging 0.9 to 2.55 microns 0.144, 0.273 or 0.288 arcsec/px 1k × 1k Hawaii HgCdTe array 2.4×2.4 to 4.9×4.9 arcmin Also does spectroscopy and imaging polarimetry.
SofI IR grism spectroscopy 0.9 to 2.55 microns R = 600 to 2200 1k × 1k Hawaii HgCdTe array Also does imaging and imaging polarimetry.

2.2m MPI telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
WFI Optical imaging 3300 to 10000 Å 0.238 arcsec/px Mosaic of eight 4k×2k CCDs 34 × 33 arcmin Readout time 27s.
FEROS Optical échelle spectroscopy 3500 to 9200 Å R = 48 000 EEV 4k×2k CCD Fibre entrances subtend 2.0 arcsec High-efficiency, fixed-format stable instrument. It has two fibres, allowing simultaneous observation of a science target and either a local sky or a ThAr wavelength calibration.

Only limited time is available on the 2.2m to visiting astronomers, as much of the time is allocated to German and Chilean research. The Max Planck Institute operate the seven-band simultaneous imager GROND, which is not a facility instrument.

 


Las Campanas Observatory (LCO)

UK astronomers have no direct access to these telescopes, but time can be obtained through collaboration with astronomers who are at some American and Chilean institutions. 50% of the time goes to Carnegie, who effectively operate the telescopes, 25% to Harvard and 10% to Chile. The remainder goes to a small number of other American institutions and to NOAO.

6.5m Magellan Baade telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
PANIC IR imaging 0.8 to 2.5 micron 0.125 arcsec/px Hawaii HgCdTe 1k × 1k array 128 × 128 arcsec
IMACS Optical wide-field imaging 3400 to 11000 Å 0.11 or 0.20 arcsec/px Mosaic of eight 4k × 2k SITe CCDs 15.5×15.5 or 27.2×27.2 arcmin Also does long-slit and multi-object spectroscopy.
IMACS Optical grating and grism spectroscopy 3400 to 11000 Å 0.068 to 2.037 Å/px Mosaic of eight 4k × 2k SITe CCDs 15.5×15.5 or 27.2×27.2 arcmin Does multi-object spectroscopy. Also does wide-field imaging.
FIRE IR échellette spectroscopy 0.82 to 2.51 microns R = 6000 - 8000

Can also work in high-throughput low-resolution mode with a prism instead of the échellette

6.5m Magellan Clay telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
MagIC Optical imaging ugriz and BVRI 0.069 arcsec/px SITe 2k × 2k CCD 142 × 142 arcsec
MagE Optical echellette spectroscopy 3100 Å to 1 micron R = 4100 for 1 arcsec slit EEV 2k × 1k CCD Slit length 10 arcsec at 0.3 arcsec/px Designed for high throughput, particularly in the blue
MIKE Optical échelle spectroscopy 3500 to 9500 Å R = 22 000 to 88 000 Two 4k × 2k CCDs; SITe in the blue camera and MIT in the red camera Capable of multi-object spectroscopy

The wide-field optical imager Megacam and the near-IR multimode instrument MMIRS are also on the Magellan telescopes for short observing runs at some times.

2.5m Irénée du Pont telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
Direct CCD Optical imaging U B V R I 0.259 arcsec/px 2k × 2k TEK CCD 8.85 × 8.85 arcmin
WIRC IR wide-field imaging 0.8 to 2.5 micron 0.196 arcsec/px Mosaic of four Hawaii HgCdTe 1k × 1k array 201×201 arcsec per detector, 12.5×12.5 arcmin for a four-exposure field Full 12.5×12.5 arcmin field requires four exposures to completely cover.
WFCCD Optical wide-field imaging 3600 to 9000 Å 0.77 arcsec/px 2k × 2k TEK CCD 25 × 25 arcmin Can do multi-object spectroscopy
B & C spectrograph Optical grating spectroscopy 3500 to 9000 Å 0.52 to 3.0 Å/px Marconi 2048 × 515 pixel CCD Maximum slit length 271 arcsec
Échelle spectrograph Optical échelle spectroscopy 3700 to 7000 Å R = 45 000 with 1 arcsec slit TEK 2k × 2k CCD

1.0m Henrietta Swope telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
Direct CCD Optical imaging U B V R I 0.435 arcsec/px 2k × 3k SITe CCD 14.8 × 22.8 arcmin
RETROCAM IR imaging 0.8 to 2.5 micron 0.54 arcsec/px Hawaii HgCdTe 1k × 1k array 9.2 × 9.2 arcmin

 


Gemini Observatory

Due to the recent funding crisis UK astronomers may soon lose access to the Gemini telescopes (see here). In addition, the Aspen programme of instrument development for Gemini has largely been abandoned for financial reasons. The GNIRS near-IR spectrograph was damaged in farcical circumstances in May 2007 (they accidentally heated it far above room temperature) but will be repaired and upgraded then offered for use on Gemini-North. New instruments are currently being worked on (the FLAMINGOS-2 near-IR multi-mode instrument, GSAOI and GPI) and a new longer-term plan is being formulated.

8.1m Gemini North (Mauna Kea, Hawaii)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
GMOS Optical imaging 3500 to 11000 Å 0.073 arcsec/px Mosaic of three 4k × 2k CCDs 5.5×5.5 arcmin Also does long-slit, multi-object or integral-field spectroscopy. The twin instrument on Gemini South has a better blue response.
GMOS Optical spectroscopy 3500 to 11000 Å 0.2 to 1.7 Å/px Mosaic of three 4k × 2k CCDs IFU has 35×35 arcsec field of view Does long-slit, multi-object, integral-field spectroscopy. Also does imaging. The twin instrument on Gemini South has a better blue response.
NIRI IR imaging 1 to 5 microns 0.022, 0.050 or 0.117 Å/px Aladin InSb 1k × 1k array 22×22, 51×51 or 120×120 arcsec Also does long-slit spectroscopy. Can use the AO system.
NIRI IR grism spectroscopy 1 to 5 microns R = 460 to 1650 Aladin InSb 1k × 1k array 22×22, 51×51 or 120×120 arcsec Also does imaging. Can use the AO system.
NIFS IR integral-field spectroscopy 0.95 to 2.40 microns R = 5000 Hawaii HgCdTe 1k × 1k array 3×3 arcsec Uses the AO system. Can do spectropolarimetry.
MICHELLE Mid-IR imaging 7 to 26 microns 0.1005 arcsec/px IBC Si:As 320 × 240 pixels array 32×24 arcsec Uses the AO system. Can do polarimetry. Can also do grating spectroscopy.
MICHELLE Mid-IR grating spectroscopy 7 to 26 microns R = 200 to 30 000 IBC Si:As 320 × 240 pixels array 0.201 arcsec/px long slit Uses the AO system. Can also do imaging.

8.1m Gemini South (Cerro Pachon, Chile)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
GMOS Optical imaging 3500 to 11000 Å 0.073 arcsec/px Mosaic of three 4k × 2k CCDs 5.5×5.5 arcmin Also does long-slit, multi-object or integral-field spectroscopy. The twin instrument on Gemini North has a better red response. Note that fringing in the red is appalling!
GMOS Optical spectroscopy 3500 to 11000 Å 0.2 to 1.7 Å/px Mosaic of three 4k × 2k CCDs IFU has 35×35 arcsec field of view Does long-slit, multi-object, integral-field spectroscopy. Also does imaging. The twin instrument on Gemini North has a better red response. Note that fringing in the red is appalling!
T-ReCS IR imaging 8 to 26 microns 0.09 Å/px Raytheon SiAs 320 × 240 pixel array 28.8×21.6 arcsec Also does long-slit spectroscopy. Can use the AO system.
T-ReCS IR grism spectroscopy 8 to 26 microns Spectral: R = 80 to 1000. Spatial: 0.09 Å/px Raytheon SiAs 320 × 240 pixel array Slit length is 21.6 arcsec Also does imaging. Can use the AO system.

 


Kitt Peak National Observatory (KPNO)

4m Mayall telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
MOSAIC imager Optical wide-field imaging 3500 to 9500 Å 0.26 arcsec/px Mosaic of eight SITe 4k × 2k CCDs 36 × 36 arcmin Read-out time 2.5 min.
R-C spectrograph Optical grating spectroscopy 3500 to 9000 Å 0.37 to 5.52 Å/px TEK 2k × 2k CCD 5.2 arcmin slit length Has multi-object capability
MARS Multi-Aperture Red Spectometer 6000 to 10000 Å 2.0 to 4.3 Å/px Lawrence Berkeley 1980×800 CCD Field of view 4 arcmin High throughput and multi-object capability
Échelle spectrograph Optical échelle spectroscopy Red optical wavelengths R = 18 000 to 80 000 Normally TEK 2k × 2k CCD
NEWFIRM IR imaging 1 to 2.3 micron 0.4 arcsec/px Mosaic of four InSb 2k × 2k pixel arrays 28×28 arcmin
SQIID IR imaging J H K L simultaneous 0.39 arcsec/px InSb 1k × 1k pixel arrays 200 arcsec (circular) Get images in the four filters simultaneously.
FLAMINGOS IR imaging J H K Ks 0.316 arcsec/px HgCdTe 2k × 2k pixel array 10×10 arcmin Can do spectroscopy too. Can also be used on the 2.1m telescope.
FLAMINGOS IR spectroscopy 0.9 to 2.5 microns 4.68 or 8.55 Å/px HgCdTe 2k × 2k pixel array Up to 10 arcmin slit width Can do imaging and multi-object spectroscopy too. Can also be used on the 2.1m telescope.
IRMOS IR multi-object spectroscopy 0.9 to 2.5 microns R = 300, 1000 or 3000 HgCdTe 1k × 1k pixel array 1 arcmin slit width

2.1m telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
CCD imager Optical imaging 3300 to 9700 Å 0.305 arcsec/px TEK 2k × 2k CCD 10.4×10.4 arcmin Read-out time 2.5 min.
GoldCam spectrograph Optical grating spectroscopy 3500 to 9000 Å 0.45 to 4.85 Å/px Ford 3k × 1k CCD 5.2 arcmin slit length
SQIID IR imaging J H K L simultaneous 0.68 arcsec/px InSb 1k × 1k pixel arrays 348 arcsec (circular) Get images in the four filters simultaneously.
FLAMINGOS IR imaging J H K Ks 0.606 arcsec/px HgCdTe 2k × 2k pixel array 20×20 arcmin Can do long-slit spectroscopy too. Can also be used on the 4m telescope.
FLAMINGOS IR spectroscopy 0.9 to 2.5 microns 4.68 or 8.55 Å/px HgCdTe 2k × 2k pixel array Up to 20 arcmin slit width Can do imaging too. Can do multi-object spectroscopy when used on the 4m telescope.

3.5m WIYN telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
MIMO (MiniMosaic) Optical wide-field imaging 3300 to 9700 Å 0.14 arcsec/px Mosaic of two SITe 4k × 2k CCDs 9.5×9.5 arcmin Each CCD has two amplifiers for readout.
OPTIC Optical PSF-shaping imaging 3300 to 9700 Å 0.14 arcsec/px Mosaic of two 4k × 2k orthogonal transfer CCDs 9.5×9.5 arcmin PSFs can be shaped arbitrarily by shifting the charge round the CCDs at will during an exposure.
Hydra Optical grating spectroscopy 3500 to 9000 Å R = 700 to 22 000 TEK 2k × 2k CCD 5.2 arcmin slit length Fibre-fed multiobject spectrograph: can do up to 100 objects. Also can do IFU with DensePak and SparsePak units.
WHIRC IR imaging J H Ks 0.1 arcsec/px VIRGO HgCdTe 2k × 2k pixel array 3.3×3.3 arcmin Can do long-slit spectroscopy too. Can also be used on the 4m telescope.

0.9m WIYN telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
MOSA (CCD Mosiac) Optical wide-field imaging 3300 to 9700 Å 0.425 arcsec/px Mosaic of eight SITe 4k × 2k CCDs 59×59 arcmin

 


Cerro Tololo Inter-American Observatory (CTIO)

The 1.5m and 1.3m telescopes are operated entirely in service/queue mode. The 1.3m was originally for 2MASS. The 1.0m is classical observing only, whereas the 0.9m is mixed classical/service observing. All four small telescope (1.5m, 1.3m, 1.0m, 0.9m) are owned and operated by the SMARTS Consortium.

4m Blanco telescope (Cerro Tololo)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
MOSAIC II Optical wide-field imaging 3400 to 10000 Å 0.27 arcsec/px Mosaic of eight SITe 4k × 2k CCDs 36 × 36 arcmin Read-out time 2.5 min using 8-channel read mode.
R-C spectrograph Optical grating spectroscopy 3500 to 11000 Å 0.48 to 3.75 Å/px Loral 3k × 1k CCD 328 arcsec slit
HYDRA Optical multi-object spectroscopy 3500 to 10000 Å 0.27 to 1.24 Å/px SITe 4k × 2k CCD 40 × 40 arcmin Also has a higher-resolution échelle grating available.
ISPI IR imaging 1 to 2.5 microns 0.3 arcsec/px Hawaii HgCdTe 2k × 2k pixel array 10.5 × 10.5 arcmin

4.1m SOAR telescope (Cerro Pachon)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
SOI Optical imaging 3100 to 10500 Å 0.077 arcsec/px Mosaic of two EEV 4k × 2k CCDs 5.25 × 5.25 arcmin
Goodman HTS Optical imaging 3200 to 8500 Å 0.15 arcsec/px Mosaic of two UL/LL 4k × 2k CCDs 5 × 5 arcmin
Goodman HTS Optical grating spectroscopy R = 1400 to 6000 0.15 arcsec/px Mosaic of two UL/LL 4k × 2k CCDs 5 × 2.5 arcmin Can do multi-object spectroscopy.
OSIRIS IR imaging 1 to 2.2 microns 0.32 or 0.13 arcsec/px Hawaii HgCdTe 1k × 1k pixel array 3.3×3.3 or 1.3×1.3 arcmin
OSIRIS IR spectroscopy 1 to 2.2 microns R = 1400 to 3000 Hawaii HgCdTe 1k × 1k pixel array 3.3×3.3 arcmin Can do multi-object spectroscopy.

1.5m telescope (Cerro Tololo)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
RC spectrograph Optical grating spectroscopy 3500 to 9000 Å resolution 2.2 to 17.2 Å Loral 1200 × 800 CCD
CPAPIR IR wide-field imaging 1.0 to 2.5 micron 1.03 arcsec/px Hawaii HgCdTe 2k × 2k array 35 × 35 arcmin

1.3m telescope (Cerro Tololo)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
ANDICAM Optical/IR imaging UBVRI and YJHK 0.185 and 0.137 arcsec/px Fairchild 2k×2k CCD and Hawaii HgCdTe 1k×1k IR array 6.3×6.3 and 2.4×2.4 arcmin Observes in the optical and IR simultaneously

1.0m telescope (Cerro Tololo)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
Y4KCAM Optical wide-field imaging UBVRI and ugriz 0.289 arcsec/px STA 4k × 4k CCD 20 × 20 arcmin Readout time 51s (unbinned) or 16s (2×2 binning) or <5s (4×4).

0.9m telescope (Cerro Tololo)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
CCD Optical imaging UBVRI and similar 0.396 arcsec/px 2k × 2k CCD 13.5 × 13.5 arcmin CCD can be read out through 1, 2 or 4 amplifiers.

 


South African Astronomical Observatory (SAAO)

There is also a 0.75m telescope with an IR JHKL photoelectric photometer and the possibility to use the UCT high-speed CCD photometer, and a 0.5m telescope with a UBVRI photoelectric photometer.

11m Southern African Large Telescope (SALT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
SALTICAM Optical imaging 3200 to 9500 Å 0.12 arcsec/px Mosaic of two EEV 4k × 2k CCDs 8×8 arcmin Optimised for the blue. Has a high-speed capability.

SALT has only recently been constructed. The Robert Stobie Spectrograph will soon be available for imaging, spectroscopy, and multi-object spectroscopy, and has been designed to have a good UV-blue performance. The High Resolution Spectrograph (HRS) is in preparation.

1.9m Radcliffe Telescope

The 1.9m telescope currently has some pointing restrictions, and cannot go north of δ = -10 degrees.

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
GratingSpec Optical grating spectroscopy 3500 to 10000 Å 0.3 to 3.2 Å/px gives 0.5 to 5.0 Å resolution SiTE 266 × 1798 CCD 24 arcsec slit
GIRAFFE Optical échelle spectroscopy 4000 to 10000 Å R = 39 000 TEK 1k × 1k CCD (cosmetic defects) (fibre-fed) Observations can be taken of the blue or red optical wavelength regions (but not simultaneously). A second fibre is available for simultaneous arc or sky spectra, but these options are normally not used.
CCD camera Optical imaging Optical wavelengths 0.12 arcsec/px TEK 1k × 1k CCD 2.5×2.5 arcmin Also used on 1m telescope.
UCT CCD Optical imaging Optical wavelengths 0.13 arcsec/px EEV 576 × 420 CCD 1.2×0.9 arcmin Has high-speed frame transfer capability. Can also be used on 1m and 0.75m telescopes.

1.0m telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
CCD camera Optical imaging Optical wavelengths 0.31 arcsec/px TEK 1k × 1k CCD 5×5 arcmin Also used on 1.9m telescope.
UCT CCD Optical imaging Optical wavelengths 0.30 arcsec/px EEV 576 × 420 CCD 2.7×2.0 arcmin Has high-speed frame transfer capability. Can also be used on 1.9m and 0.75m telescopes.

 


Anglo Australian Observatory (AAO) (Siding Springs)

3.9m Anglo Australian Telescope (AAT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
AAOmega Optical multi-object spectroscopy 3700 to 8500 Å R = 1200 to 10000 Mosaic of two 4k × 2k CCDs Field of view is 2 degrees, fibres have 2 arcsec entrance. Can observe 392 objects simultaneously. Can also do integral-field spectroscopy (512 fibres covering 22×11 arcsec).
IRIS2 IR imaging 0.9 to 2.5 microns 0.45 arcsec/px HgCdTe 1k × 1k array 7 × 7 arcmin Also does imaging. Can use the AO system.
IRIS2 IR grism spectroscopy 0.9 to 2.5 microns R = 2400 HgCdTe 1k × 1k array 7 × 7 arcmin Does multi-object or long-slit spectroscopy.
UCLES Optical échelle spectroscopy Optical wavelengths R = 40 000 to 120 000 Choice of EEV 4k × 2k CCD (blue-sensitive) or MIT-LL 4k × 2k CCD (red-sensitive) Choice of two dispersive gratings.
UHRF Optical échelle spectroscopy Optical wavelengths R = 300 000, 600 000 or 940 000 EEV 4k × 2k CCD Wavelength coverage 4 to 45 Å Red-sensitive MIT-LL CCD is available but its lack of binning means it is not as suitable as the EEV chip (which is normally binned 8×8 for the UHRF).