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
| Optical imaging |
| Optical spectroscopy |
| Optical échelle spectroscopy |
| Infrared imaging |
| Infrared spectroscopy |
| Infrared échelle spectroscopy |
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Optical wavelengths | Infrared wavelengths | ||||
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Imaging | Spectroscopy | Échelle spec. | Imaging | Spectroscopy | Échelle spec. |
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La Palma (Spain) | |||||
WHT 4.2m | ACAM | ISIS WYFFOS ACAM |
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LIRIS | LIRIS | |
INT 2.5m | WFC | IDS | |
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NOT 2.5m | ALFOSC MOSCA StanCam | ALFOSC | FIES | NOTCAM |
NOTCAM |
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TNG 3.6m | DOLORES | DOLORES | HARPS-North | NICS | NICS | |
LT 2.0m | RATCam RISE RINGO3 IO:O | FRODOspec | |
IO:I |
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GTC 10.4m | OSIRIS | OSIRIS | |
CanariCam | CanariCam | |
TCS (Teide) | FastCam | |
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CAIN-3 | |
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Calar Alto (Spain) | |||||
3.5m | LAICA MOSCA | MOSCA PMAS TWIN | |
Omega-2000 | |
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2.2m | BUSCA CAFOS AstraLux | CAFOS | CAFE | MAGIC | MAGIC | |
1.23m | CCD | |
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Haute-Provence and Pic du Midi (France) | |||||
OHP 1.93m | |
CARELEC | SOPHIE | |
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TBL 2.0m | |
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NARVAL | |
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CFHT (Hawaii) | |||||
3.6m CFHT | WFCAM | |
ESPaDOnS | WIRCAM | |
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European Southern Observatory (Paranal, Chile) | |||||
VLT UT1 | FORS2 | FORS2 | |
NACO | NACO KMOS | |
VLT UT2 | X-SHOOTER FLAMES | UVES FLAMES / UVES |
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X-SHOOTER | |
VLT UT3 | VIMOS SPHERE/ZIMPOL |
VIMOS | |
VISIR SPHERE/IRDIS |
VISIR SPHERE/IRDIS SPHERE/IFS |
VISIR |
VLT UT4 | |
MUSE | |
HAWK-I | SINFONI | |
VISTA | |
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VIRCAM | |
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VST | OmegaCAM | |
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European Southern Observatory (La Silla, Chile) | |||||
3.6m | |
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HARPS | |
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NTT 3.6m | EFOSC | EFOSC | |
SofI | SofI | |
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South African Astronomical Observatory (Sutherland, SA) | |||||
SALT | SALTICAM BVIT | RSS | |
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1.9m Radcliffe | CCD UCT | GratingSpec | GIRAFFE | |
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1.0m | CCD UCT | |
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Australian Astronomical Observatory (Siding Springs, Australia) | |||||
4.0m AAT | |
AAOmega HERMES | UCLES UHRF | IRIS2 | IRIS2 | |
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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 | |
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WIYN 0.9m | MOSAIC | |
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Cerro Tololo Inter-American Observatory (Chile) | |||||
4m Blanco | DECam | HYDRA | |
ISPI | |
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4.1m SOAR | SOI HTS | HTS | |
OSIRIS SPARTAN |
OSIRIS | |
1.5m | |
R-C | CHIRON | |
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1.3m | ANDICAM | |
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ANDICAM | |
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1.0m | Y4KCAM | |
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0.9m | CCD | |
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Imaging | Spectroscopy | Échelle spec. | Imaging | Spectroscopy | Échelle spec. |
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Optical wavelengths | Infrared wavelengths |
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 |
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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. |
| Optical imaging |
| Optical spectroscopy |
| Optical échelle spectroscopy |
| Infrared imaging |
| Infrared spectroscopy |
| Infrared échelle spectroscopy |
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.
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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. |
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. |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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. |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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. |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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 |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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 | |
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.
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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 |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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.
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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 |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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 |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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) |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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.
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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. |
Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
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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 |
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. |
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. |
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 |
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.
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. |
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. |
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.
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 |
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. |
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. |
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 |
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.
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 |
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. |
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. |
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 |
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). |
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. |
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.
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.
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. |
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. |
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). |