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, except for LCOGT which has still to be added.
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 ----
TCS
Northern hemisphere (other):
CAHA:
3.5m
2.2m
1.23m ----
OHP:
1.93m
1.20m ----
TBL 2.0m ----
Aristarchos 2.3m ----
CFHT
Southern hemisphere (ESO):
Paranal:
VLT1
VLT2
VLT3
VLT4
VISTA
VST ----
La Silla:
3.6m
NTT
2.2m MPI
Southern hemisphere (other):
SAAO:
SALT
1.9m
1.0m ----
AAT
US facilities (apply via NOAO):
KPNO:
4m
WIYN 3.5
WIYN 0.9 ----
CTIO:
4.0m
SOAR
1.3m
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 ACAM WEAVE |
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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 GIARPS |
NICS | NICS | GIANO GIARPS |
| LT 2.0m | RISE MOPTOP IO:O |
FRODOspec SPRAT |
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IO:I |
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| TCS (Teide) | FastCam MUSCAT2 |
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Calar Alto (Spain) | |||||
| 3.5m | LAICA | PMAS | CARMENES | Omega-2000 | |
CARMENES |
| 2.2m | BUSCA CAFOS AstraLux |
CAFOS | CAFE | |
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| 1.23m | CCD | |
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Haute-Provence and Pic du Midi (France) | |||||
| OHP 1.93m | |
CARELEC | SOPHIE | |
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| OHP 1.20m | CCD | |
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| TBL 2.0m | |
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Neo-NARVAL | |
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Helmos (Greece) | |||||
| 2.3m Aristarchos | LN LN2 RISE2 | |
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CFHT (Hawaii) | |||||
| 3.6m CFHT | WFCAM | SITELLE | ESPaDOnS | WIRCAM | |
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European Southern Observatory (Paranal, Chile) | |||||
| VLT ICCF | |
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ESPRESSO | |
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| VLT UT1 | FORS2 | FORS2 | |
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KMOS | |
| VLT UT2 | FLAMES / GIRAFFE | UVES FLAMES / UVES |
VISIR | VISIR | |
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| VLT UT3 | SPHERE/ZIMPOL X-SHOOTER |
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SPHERE/IRDIS | SPHERE/IRDIS SPHERE/IFS |
X-SHOOTER |
| VLT UT4 | |
MUSE | |
HAWK-I | |
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| 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 | EFOSC2 ULTRACAM |
EFOSC2 | |
SofI | SofI | |
| 2.2m MPI | WFI | |
FEROS | |
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| 0.6m REM | ROS2 | |
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REMIR | |
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South African Astronomical Observatory (Sutherland, SA) | |||||
| SALT | SALTICAM BVIT |
RSS | HRS | |
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| 1.9m Radcliffe | CCD SHOC HIPPO |
SpUpNIC | |
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| 1.0m | CCD SHOC |
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Australian Astronomical Observatory (Siding Springs, Australia) | |||||
| 4.0m AAT | |
AAOmega HERMES |
Veloce | |
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Kitt Peak National Observatory (Arizona, USA) | |||||
| 4m Mayall | MOSAIC-3 | KOSMOS | |
NEWFIRM | |
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| WIYN 3.5m | ODI | Bench spectrograph | |
WHIRC | |
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| WIYN 0.9m | HDI | |
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Cerro Tololo Inter-American Observatory (Chile) | |||||
| 4m Blanco | DECam | COSMOS | |
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ARCoIRS |
| 4.1m SOAR | SOI Goodman |
Goodman | |
SPARTAN | |
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| 1.3m | ANDICAM | |
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ANDICAM | |
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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 |
|---|---|---|---|
| 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. The 2.2m MPI telescope at La Silla is only available via OPTICON. |
| 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 and 1.20m telescopes. |
| 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 all three telescopes. |
| Aristarchos | ~28 August | March to June July to October November to February |
UK astronomers can apply via OPTICON. |
| REM | ~28 August ~28 February |
1 April to 31 August 1 September to 31 March |
UK astronomers can apply via OPTICON. |
| CFHT | ~28 August ~28 February |
1 February to 31 July 1 August to 31 January |
UK astronomers can apply via OPTICON. |
| SAAO | 15 September 15 January 15 May |
January to April May to August September 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). |
| | 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 |
| WEAVE | Multi-object fibre spectroscopy | Low res: 3660-6060 Å and 5790-9590 Å High res: 4040-4650 or 4730-5450 Å and 5950-6850 Å |
Low resolution: R = 5000 High resolution: R = 20000 |
Two 6k × 6k EEV CCDs in each arm | Field of view is 2 degrees. Fibre diameter is 1.3 arcsec |
Has 1900 fibres in total. Observes in the blue and red arms simultaneously |
| 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 WHT will shortly be moving to a new operational scheme whereby the WEAVE survey instrument will take up about 70% of the time, and the remainder of the time will be available for ISIS, LIRIS, ACAM and visiting instruments.
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| 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. |
| 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. |
The INT will host the HARPS3 spectrograph from the second half of 2021 (date subject to change). Once HARPS3 has been installed, IDS and WFC will be mothballed and likely never used again.
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| 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). |
| 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. Has two diffusers to do photometry of bright sources. |
| 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. |
| FIES | Optical échelle spectroscopy | 4000 to 8300 Å | R = 25 000, 45 000 or 65 000 | EEV 2k × 2k CCD | 1.3 or 2.5 arcsec (circular fibres) 1.5 or 2.6 arcsec (octagonal fibres) |
Poor response in the blue. Can do a simultaneous Th-Ar calibration. |
| 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 |
| 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. | |
| GIANO | IR échelle spectroscopy | 0.95 to 2.45 μm | R = 50 000 | HAWAII2 2k × 2k CCDs | Fibre opening is 1 arcsec diameter. | Simultaneous Th-Ar mode allows wavelength stability of 0.5 m/s. |
| GIARPS | Optical+IR échelle spectroscopy | 3830 to 6900 Å 0.95 to 2.45 μm |
R = 115 000 R = 50 000 |
Two EEV 4k × 2k CCDs HAWAII2 2k × 2k CCDs |
Fibre opening is 1 arcsec diameter. | Is HARPS-North and GIANO used simultaneously on the same target |
| 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 | |
| RISE | Optical high-speed imaging | 7200 Å long-pass filter (roughly I+z) | 0.54 arcsec/px | EEV frame-transfer CCD | 9.2 × 9.2 arcmin | Readout speed is "less than a second". |
| MOPTOP | Optical high-speed polarimetry | tbc | tbc | Two 4.2Mpx Andor Zyla sCMOS detectors | 8 arcmin | Readout speeds from 0.1 to 1 Hz. |
| 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. |
| SPRAT | Optical spectroscopy | 4000 to 8000 Å | Dispersion 4.6 Å/px, resolution approx 18 Å |
Andor iDus CCD | 1.8 × 95 arcsec slit | Low-resolution and high-throughput for observing transients |
| IO:I | Infrared imaging | H filter (could change to J in future semesters) | 0.184 arcsec/px | 2k × 2k Hawaii HgCdTe array | 6.3 × 6.3 arcmin | |
| 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 | |
| MUSCAT2 | Simultaneous 3-band imaging | griz filters | 0.435 arcsec/px | Princeton Instruments 1024×1024 pixel CCDs | 7.4 × 7.4 arcmin | Simultaneous imaging in three bands. Band 1: g or r. Band 2: i. Band 3: z. |
| 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. |
| 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 | |
| CARMENES | Optical+IR échelle spectroscopy | VIS channel: 520 to 960 nm NIR channel: 960 to 1710 nm |
R = 82 000 | 4k×4k e2v CCD (VIS) and two 2k×2k Hawaii-2RG (NIR) | Fibre feed | VIS and NIR arms operate simultaneously |
| OMEGA-2000 | Wide-field IR imaging | zJHK | 0.45 arcsec/px | HgCdTe 2k × 2k array | 15.4 × 15.4 arcmin | Mounted at prime focus. |
| 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 |
| 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. |
| 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 |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| CCD imager | Optical imaging | |
0.38 arcsec/px | Andor iKon L936 | 13.1 × 13.1 arcmin | |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| Neo-NARVAL | Optical échelle spectroscopy | 3700 to 10000 Å | R = 65 000 | tbc | Fibre-fed | High stability allows velocity measurements to 3 m/s |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| LN | Optical imaging | Optical | 0.28 arcsec/px | 1k×1k SITe CCD | 4.8 × 4.8 arcmin | |
| LN2 | Optical imaging | Optical | 0.16 arcsec/px | 2k×2k e2v CCD | 5.5 × 5.5 arcmin | |
| RISE2 | High-speed imaging | V+R filter | 0.6 arcsec/px | 1k×1k e2v EMCCD | 10 × 10 arcmin | |
| ATS | Optical spectroscopy | 4000 to 7250 Å | 1.3 to 3.2 Å | 1k×1k Apogee CCD | 10 arcsec fibre bundle | Transient object spectroscopy |
| 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) |
| SITELLE | Optical integral-field spectroscopy | 350 to 900 nm | R = 1 to 10 000 | Two 2k×2k CCDs | 11 × 11 arcmin field | 0.32 arcsec/pixel well samples the typical 0.8 arcsec seeing at this telescope |
| 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 |
|---|---|---|---|---|---|---|
| ESPRESSO | Optical échelle spectroscopy | 3800 to 7750 Å | MR: 70 000 HR: 140 000 UHR: 190 000 |
Blue: 3800-5200 Å Red: 5200-7750 Å Both are e2v 9k×9k CCDs |
MR: 1 arcsec fibre HR: 1 arcsec fibre UHR: 0.5 arcsec fibre |
HR and UHR each use one VLT Unit Telescope (UT). MR uses all four UTs simultaneously. Wavelength calibration is by a laser frequency comb. |
| 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. |
| 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. |
| 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: 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. |
| 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 | Previously on UT4 |
| VISIR | Mid-IR spectroscopy | 8-13 and 17-24 microns | R = 350, 3200 or 25000 | 1k×1k Raytheon Aquarius IBC | 32 arcsec long slit | Previously on UT4 |
| 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%. |
| SPHERE/ZIMPOL | Extreme-AO and coronagraphic imaging and polarimetry | 500 to 900 nm | 7 mas per pixel | CCD | 3.5×3.5 arcsec | Unavailable from November 2018. |
| 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 |
| 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 |
|---|---|---|---|---|---|---|
| ULTRACAM | Optical high-speed simultaneous three-band imaging | u in blue arm, g in green arm, choice of r,i,z in red arm | 0.35 arcsec/px | Three 1k × 1k frame-transfer CCDs | 6 × 6 arcmin | Operates as a PI instrument, not a common-user instrument. |
| EFOSC2 | Optical imaging | 3500 to 11000 Å | 0.12 arcsec/px | Loral 2k × 2k CCD | 4.1 × 4.1 arcmin | Also does long-slit and multi-object spectroscopy and polarimetry. |
| EFOSC2 | Optical grism spectroscopy | 3200 to 11000 Å | 0.92 to 6.66 Å/px VPH: R = 4000 |
Loral 2k × 2k CCD | Up to 4.1 × 4.1 arcmin depending on grism | 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. |
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 |
|---|---|---|---|---|---|---|
| WFI | Simultaneous optical and IR imaging | g, r, i, z 1 to 2.3 μm |
0.58 arcsec/px (optical) 1.2 arcsec/px (IR) |
One optical CCD and one Hawaii IR detection | 9.1 × 9.1 arcmin | Robotic operation. Five bands observed simultaneously (g, r, i, z plus one IR band) |
| 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 four LBNL 4k × 4k CCDs | 36 × 36 arcmin | Read-out time 30 or 40s. |
| KOSMOS | Optical single or multi-object spectroscopy | 3500 to 10275 Å | R ≈ 660 to 3300 | E2V or LBNL CCD | 5 × 10 arcmin | Has multi-object capability |
| NEWFIRM | IR imaging | 1 to 2.3 micron | 0.4 arcsec/px | Mosaic of four InSb 2k × 2k pixel arrays | 28×28 arcmin |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| ODI | Optical wide-field imaging | 3300 to 9700 Å | 0.11 arcsec/px | Mosaic of thirty OTA CCDs | 1 square degree (approximately half-filled) | The CCDs are orthogonal transfer |
| Bench spectrograph | Optical multi-object spectroscopy | 3500 to 9000 Å | 0.15 to 8.9 Å | STA1 2600×4000 CCD | Up to 1 degree field (with HYDRA) | Fed by HYDRA (up to 100 objects). Also can do IFU with HexPak, GradPak 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 |
|---|---|---|---|---|---|---|
| HDI | Optical wide-field imaging | 3300 to 9700 Å | 0.43 arcsec/px | 4k × 4k CCD | 29.2 × 29.2 arcmin | Name: Half Degree Imager |
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. |
| COSMOS | Optical single or multi-object spectroscopy | 3500 to 10275 Å | R ≈ 660 to 3300 | E2V or LBNL CCD | 5 × 10 arcmin | Has multi-object capability |
| ARCoIRIS | IR échelle spectroscopy | 0.80 to 2.47 microns | R ≈ 3500 | Hawaii HgCdTe 2k × 2k array | slit width 1.1 arcsec, length 28 arcsec | all wavelength range is observed simultaneously |
| 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 | Optical imaging | 3200 to 8500 Å | 0.15 arcsec/px | Mosaic of two UL/LL 4k × 2k CCDs | 7.2 arcmin diameter circle | |
| Goodman | 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 | 0.066 or 0.040 arcsec/px | Four Hawaii HgCdTe 2k × 2k arrays | 5.04×5.04 or 3.05×3.05 arcmin |
| 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 |
|---|---|---|---|---|---|---|
| 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. |
| 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. |
| HRS | Optical échelle spectroscopy | 3700 to 8900 Å | R = 14 000, 40 000 or 65 000 | 2k×4k CCD (blue arm) and 4k×4k CCD (red arm) | 1.6 and 2.2 arcsec diameter optical fibres | The blue and red arms operate simultaneously |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| SHOC | Optical imaging | Optical wavelengths | 0.076 or 0.163 arcsec/px | 1k × 1k Andor frame-transfer EMCCD | 1.29×1.29 arcmin or 2.79×2.79 arcmin | Larger field of view needs the focal reducer |
| HIPPO | Optical imaging and polarimetry | Optical wavelengths | photomultiplier tubes | photomultiplier tubes | two apertures available | |
| SpUpNIC | Optical grating spectroscopy | 3500 to 10000 Å | 0.5 to 5.0 Å resolution | CCD | n/a |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| STE4 CCD camera | Optical imaging | UBVRI, ugriz, and narrow-band filters | 0.31 arcsec/px | STE4 1k × 1k CCD | 5.3×5.3 arcmin | Not currently available on the 1.9m telescope. |
| STE3 CCD camera | Optical imaging | UBVRI, ugriz, and narrow-band filters | 0.31 arcsec/px | STE3 512 × 512 CCD | 2.6×2.6 arcmin | Not currently available on the 1.9m telescope. |
| SHOC | Optical imaging | Optical wavelengths | 0.167 arcsec/px | 1k × 1k Andor frame-transfer EMCCD | 2.85 × 2.85 arcmin | |
| 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 |
| Veloce | Optical échelle spectroscopy | 5800 to 9300 Å | R = 80 000 | Red-optimised CCD | 2.5 arcsec IFU with 26 hexagonal fibres | Wavelength calibration via laser comb and/or a Th-U-Xe arc lamp |
