Optical/infrared telescopes available to UK astronomers (2015 March)

 

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. Specialist instruments such as interferometers and coronographers are not included. 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 includes all of the telescopes available via OPTICON.
Quite a few other telescopes not included here (e.g. Keck, Magellan, LBT) offer small numbers of nights to the general astronomical community through various schemes.

 

Northern hemisphere (La Palma):     WHT     INT     ----     NOT     ----     TNG     ----     LT     ----     GTC     ----     TCS
Northern hemisphere (other):         CAHA:     3.5m     2.2m     1.23m     ----     OHP 1.93m     ----     TBL 2.0m     ----     CFHT
Southern hemisphere (ESO):         Paranal:     VLT1     VLT2     VLT3     VLT4     VISTA     VST     ----     La Silla:     3.6m     NTT
Southern hemisphere (other):         SAAO:     SALT     1.9m     1.0m     ----     AAT    
US facilities (apply via NOAO):         KPNO:     4m     2.1m     WIYN 3.5     WIYN 0.9     ----     CTIO:     4.0m     SOAR     1.5m     1.3m     1.0m     0.9m

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 ACAM ISIS   WYFFOS
ACAM
LIRIS LIRIS
  INT 2.5m WFC IDS



  NOT 2.5m ALFOSC   MOSCA   StanCam ALFOSC FIES NOTCAM
NOTCAM

  TNG 3.6m DOLORES DOLORES HARPS-North NICS NICS
  LT 2.0m RATCam   RISE   RINGO3   IO:O FRODOspec
IO:I


  GTC 10.4m OSIRIS OSIRIS
CanariCam CanariCam
  TCS (Teide) FastCam

CAIN-3

 
  		      Calar Alto   (Spain)
  3.5m LAICA   MOSCA MOSCA   PMAS   TWIN
Omega-2000

  2.2m BUSCA   CAFOS   AstraLux CAFOS CAFE MAGIC MAGIC
  1.23m CCD




 
  		      Haute-Provence and Pic du Midi   (France)
  OHP 1.93m
CARELEC SOPHIE


  TBL 2.0m

NARVAL


 
  		      CFHT   (Hawaii)
  3.6m CFHT WFCAM
ESPaDOnS WIRCAM

 
  		      European Southern Observatory   (Paranal, Chile)
  VLT UT1 FORS2 FORS2
NACO NACO   KMOS
  VLT UT2 X-SHOOTER   FLAMES UVES
FLAMES / UVES

X-SHOOTER
  VLT UT3 VIMOS
SPHERE/ZIMPOL 		VIMOS
VISIR
SPHERE/IRDIS 		VISIR
SPHERE/IRDIS
SPHERE/IFS 		VISIR
  VLT UT4
MUSE
HAWK-I SINFONI
  VISTA


VIRCAM

  VST OmegaCAM




 
  		      European Southern Observatory   (La Silla, Chile)
  3.6m

HARPS


  NTT 3.6m EFOSC EFOSC
SofI SofI
 
  		      South African Astronomical Observatory (Sutherland, SA)
  SALT SALTICAM   BVIT RSS



  1.9m Radcliffe CCD   UCT GratingSpec GIRAFFE


  1.0m CCD   UCT




 
  		      Australian Astronomical Observatory   (Siding Springs, Australia)
  4.0m AAT
AAOmega   HERMES UCLES   UHRF IRIS2 IRIS2
 
  		      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 DECam HYDRA
ISPI

  4.1m SOAR SOI   HTS HTS
OSIRIS
SPARTAN 		OSIRIS
  1.5m
R-C CHIRON


  1.3m ANDICAM

ANDICAM

  1.0m Y4KCAM




  0.9m CCD




 

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) 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.
  ESO ~31 March
~27 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.
  LT ~15 September
4 April 		1 February to 31 July
1 August to 31 January 		UK astronomers have a share on this telescope through PATT.
  AAT ~28 August
~28 February 		1 February to 31 July
1 August to 31 January 		UK astronomers can apply via OPTICON.
  NOT ~28 August
~28 February 		1 October to 31 March
1 April to 31 September 		UK astronomers can apply via OPTICON.
  TNG ~28 August
~28 February 		1 August to 31 January
1 February to 30 July 		UK astronomers can apply via OPTICON.
  TCS (Teide) ~28 August
~28 February 		1 August to 31 January
1 February to 30 July 		UK astronomers can apply via OPTICON.
  OHP ~28 August
~28 February 		1 March to 31 August
1 September to 28 February 		UK astronomers can apply via OPTICON for the 1.93m telescope only.
  Calar Alto ~1 September
~1 March 		1 July to 31 December
1 Jan to 30 June 		UK astronomers can apply via OPTICON.
Observing time can be bought at the 2.2m and 1.23m telescopes.
  CFHT ~28 August
~28 February 		1 February to 31 July
1 August to 31 January 		UK astronomers can apply via OPTICON.
  SAAO ~1 October
~1 January
~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 does not apply to SALT.
  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).
  GTC
Large programs only (10+ nights) The GTC is no longer available through ESO.

 

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
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 prime focus 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 prime focus is in use, so is good for over-rides and ToOs.
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 is available. 		3.7 arcmin slit length It has a dichroic, and does observations in the blue and red arms simultaneously
AF2/WYFFOS Multi-object spectroscopy 3700 to 10000 Å 0.06 to 2.9 Å/px Red+4 4k×4k CCD
The old EEV mosaic can be used if justified 		20 arcmin unvignetted Uses ISIS gratings (or échelle). Up to 150 fibres available.
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

Note that the AO instrument suite (NAOMI, OASIS, INGRID and OSCA) are no longer offered as of semester 2015A, so no more applications can be made to use these instruments. PFIP will be replaced with a new instrument, PAUCam, on probably the same timescale. See here for a page summarising a community poll organised by ING as part of their planning process.

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 or
REDPLUS 4k × 2k 		3.3 arcmin slit width 235mm camera is available.
500mm camera no longer 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 is now available.

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. Can do a simultaneous Th-Ar calibration.

3.6m Telescopio Nazionale Galileo (TNG)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
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).
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.
HARPS-North Optical échelle spectroscopy 3830 to 6900 Å R = 115 000 Two EEV 4k × 2k CCDs Fibre opening is 1 arcsec diameter. Simultaneous Th-Ar mode allows wavelength stability of 0.5 m/s.
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.

2.0m robotic Liverpool Telescope (LT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
IO:O Optical imaging ugriz, BV, Hα filters 0.15 arcsec/px Fairchild 4k × 4k CCD 10 × 10 arcmin Simultaneous optical (IO:O) and infrared (IO:I) imaging is 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".
RINGO3 Optical simultaneous three-band high-speed polarimetry Blue (3500 to 6400 Å), green (6500 to 7600 Å), red (7700 to 10000 Å) 0.47, 0.47, 0.49 arcsec/px Three electron-multiplying CCDs, 512×512 pixels 4.3, 4.2, 5.1 arcmin diameter (unvignetted field) Does imaging polarimetry using a rotating polaroid in three passbands simultaneously. The passbands are separated by dichroics.
FRODOspec Optical spectroscopy 3900 to 9400 Å R = 2200 to 5500 CCDs 11 × 11 arcsec Integral-field spectrograph. The red and blue arms can be used simultaneously.
IO:I Infrared imaging JH filters 0.18 arcsec/px 2k × 2k Hawaii HgCdTe array 6 × 6 arcmin Simultaneous optical (IO:O) and infrared (IO:I) imaging is available.

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

 

Mount Teide

1.5m Telescope Carlos Sánchez (TCS)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
FastCam Lucky Imaging I band 0.01 arcsec/px Andor 512×512 pixel CCD 6 × 6 arcseconds
CAIN-3 Near-IR imaging 1 to 2.5 microns 1.0 or 0.39 arcsec/px 256 × 256 pixel HgCdTe array 4.3×4.3 or 1.7×1.7 arcmin

 

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 not butted together, so four observations are needed to fully cover one field.
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.
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
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-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 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.
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.
CAFE Optical échelle spectroscopy 3900 to 9600 Å (provisional) R = 40 000 to 60 000 (provisional) Andor 2k×2k CCD Has a target and a sky fibre. Fibre entrances subtend 2.4 arcsec Commissioned in May 2011 and details still to be confirmed
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 0.32 arcsec/px DLR-MkIII e2v CCD 16 × 16 arcmin (BVRI)
11 × 11 arcmin (other CAHA filters) 		Operated remotely and available for a given cost per night.

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.

 

Observatoire de Haute-Provence

1.93m telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
CARELEC Long-slit spectroscopy 3500 to 9000 Å R = 450 to 5400 EEV 2k × 1k CCD 5.5 arcmin slit length  
SOPHIE Optical échelle spectroscopy 3872 to 6943 Å R = 75 000 or 40 000 EEV 4k × 2k CCD Fibre-fed High stability for velocity measurements to 3-4 m/s

 

Observatoire Pic du Midi

2.0m Télescope Bernard Lyot

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
NARVAL
(see also here) 		Optical échelle spectropolarimetry 3700 to 10000 Å R = 65 000 (pol)
R = 80 000 (spec) 		EEV 4.5k × 2k CCD Fibre-fed High stability allows velocity measurements to 10-20 m/s

 

3.6m Canada-France-Hawaii Telescope (CFHT)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
MegaPrime/MegaCam Optical wide-field imaging ugriz 0.187 arcsec/px Mosaic of 36 2k×4.6k CCDs arranged in a 4×9 matrix 0.96 × 0.94 degrees CCD mosaic is tightly packed (CCDs are separated by a small fraction of their individual sizes)
ESPaDOnS
(main homepage) 		Optical échelle spectropolarimetry 3700 to 10000 Å R = 68 000 (pol)
R = 80 000 (spec) 		EEV 4.5k × 2k CCD Fibre-fed High stability allows velocity measurements to 10-20 m/s
WIRCAM Infrared wide-field imaging YJHKs 0.306 arcsec/px Mosaic of four HAWAII 2k × 2k arrays 21.5 × 21.5 arcmin CCD mosaic is tightly packed (CCDs are separated by a small fraction of their individual sizes)

 

European Southern Observatory (ESO)

Paranal observatory (VLT)

8.2m VLT Unit Telescope 1 (Antu)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
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.
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.
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.
KMOS IR multiple integral field spectroscopy 0.8 to 2.5 μm R = 2000-4200 Three HgCdTe 2k×2k Hawaii detectors 24 IFUs, each 2.8×2.8 arcsec 24 deployable IFUs each cover 2.8×2.8 arcsec in a 14×14 pixel layout.

The CRIRES infrared échelle spectrograph is out of action until 2017 for upgrading to a cross-dispersed configuration.

8.2m VLT Unit Telescope 2 (Kueyen)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
X-SHOOTER Simultaneous optical-IR échelle spectroscopy 3000 to 5595 Å,
5595 to 10240 Å,
10240 to 24800 Å 		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 0.3 to 2.5 μm in one exposure using three arms. Optimised for throughput, with a total efficiency of 30%.
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: EEV 4k×2k CCD
Red: Mosaic of two 4k×2k CCDs 		Long slit length 10 arcsec maximum. Has a blue and a red arm, which can either operated separately or simultaneously using a dichroic.

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 8-13 and 17-24 microns 0.045 or 0.076 arcsec/px 1k×1k Raytheon Aquarius IBC 40×40 or 62×62 arcsec
VISIR Mid-IR spectroscopy 8-13 and 17-24 microns R = 350, 3200 or 25000 1k×1k Raytheon Aquarius IBC 32 arcsec long slit
SPHERE/ZIMPOL Extreme-AO and coronagraphic imaging and polarimetry 500 to 900 nm 7 mas per pixel CCD 3.5×3.5 arcsec
SPHERE/IRDIS Extreme-AO and coronagraphic imaging 0.95 to 2.32 microns 12.25 mas pixel scale 2k×1k Hawaii II RG 11×11 arcsec IRDIS and IFS can observe simultaneously using a dichroic to split the light
SPHERE/IRDIS Extreme-AO and coronagraphic long-slit spectroscopy 0.95 to 2.32 microns R = 50 or R = 350 2k×1k Hawaii II RG 11 arcsec slit (spec) IRDIS and IFS can observe simultaneously using a dichroic to split the light
SPHERE/IFS Extreme-AO and coronagraphic integral-field spectroscopy 0.95 to 1.65 microns R = 50 or R = 30 2k×2k Hawaii II RG 1.73×1.73 arcsec at 12.25 mas per spaxel IRDIS and IFS can observe simultaneously using a dichroic to split the light

8.2m VLT Unit Telescope 4 (Yepun)

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
MUSE Optical integral field spectroscopy 500 nm to 900 nm R = 1750 at 500 nm to R = 3500 at 900 nm 24 4k×4k MIT/LL CCDs 1×1 arcmin at present Will have adaptive optics in future.
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
SINFONI IR integral field spectroscopy 1.1 to 2.45 microns Spatial: 0.025-0.25 arcsec. Spectral: R = 1500 to 4000 2k × 2k Hawaii 2RG detector 8×8 or 3×3 or 0.8×0.8 arcsec Has adaptive optics.

4m VISTA Visible and Infrared Survey Telescope for Astronomy

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
VIRCAM 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.

2.6m VST VLT Survey Telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
OmegaCAM Optical wide-field imaging U B V R I z 0.21 arcsec/px Mosaic of 32 4k×2k CCDs 1×1 degrees

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.

 

La Silla Observatory

3.6m telescope

Instrument Mode Wavelength coverage Resolution Detector Field of view Details
HARPS Optical échelle spectroscopy 3780 to 6910 Å R = 120 000. Also has wider fibre for higher throughput. Two EEV 4k × 2k CCDs Fibre opening is 1 arcsec diameter. Simultaneous Th-Ar 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
VPH: 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 instrument. A second fibre can be used for simultaneous sky or ThAr observations.

As of P92 (October 2013 to March 2014) the 2.2m telescope is no longer available via ESO's standard application process.

The Max Planck Institute operate the seven-band simultaneous imager GROND, which is not a facility instrument.

 

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
DECam Optical very-wide-field imaging grizy filter s 0.27 arcsec/px Mosaic of 62 SITe 2k×4k CCDs 2.2 degree field (3.0 deg.sq. in total) For the Dark Energy Survey project.
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.
SPARTAN IR imaging JHK 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 imaging 1 to 2.2 microns 0.043 or 0.073 arcsec/px Four Hawaii HgCdTe 2k×2k arrays 3.0×3.0 or 5.0×5.0 arcmin
OSIRIS IR spectroscopy 1 to 2.5 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
CHIRON Optical échelle spectroscopy 4100 to 8700 Å R = 80 000 EEV 4k×4k CCD Fibre entrance subtends 2.7 arcsec Fixed-format instrument intended for radial velocity work, and can reach 1 m/s.

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.
BVIT Optical high-speed imaging 4000 to 8500 Å 30 microns at the focal plane Super Gen II photocathode 1.9×1.9 arcmin
Robert Stobie Spectrograph Optical slit spectroscopy 3200 to 9000 Å R = 250 to 5500 (up to 9000 with a 0.6 arcsec slit) Mosaic of two EEV 4k × 2k CCDs 8 arcmin slit length Optimised for the blue.

SALT has only recently been constructed. The High Resolution Spectrograph (HRS) is in preparation.

1.9m Radcliffe Telescope

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) A second fibre is available for simultaneous arc or sky spectra.
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.

 

Australian Astronomical Observatory (AAO) (Siding Springs)

3.9m Australian Astronomical 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. Fed by either 2dF (392 deployable fibres) or KOALA (1000-element integral-field unit covering 24×18 or 32×32 arcsec).
HERMES Optical multi-object spectroscopy Simultaneous observations at 4715-4900Å, 5649-5873Å, 6478-6737Å and 7585-7887Å R = 28000, or R=50000 with a narrow slit Mosaic of two 4k × 2k CCDs Field of view is 2 degrees Fed by the 2dF fibre positioner, which places up to 392 fibres in the field of view
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) The CYCLOPS fibre feed has a diameter of 3 arcsec on the sky 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 cannot be binned (EEV chip is binned 8×8 for UHRF).