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 now 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
Northern hemisphere (other):
CAHA:
3.5m
2.2m
1.2m ----
OHP 1.93m ----
TBL 2.0m ----
UKIRT ----
Gemini North ----
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 ----
Gemini South
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 |
| |
Optical wavelengths | Infrared wavelengths | ||||
| |
Imaging | Spectroscopy | Échelle spec. | Imaging | Spectroscopy | Échelle spec. |
| |
La Palma (Spain) | |||||
| WHT 4.2m | PFIP ACAM | ISIS WYFFOS OASIS ACAM |
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INGRID 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 OIC | DOLORES | SARG | NICS | NICS | |
| LT 2.0m | RATCam RISE RINGO2 IO:O IO:THOR | FRODOspec | |
IO:I |
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| GTC 10.4m | OSIRIS | OSIRIS | |
CanariCam | CanariCam | |
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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 | |
| 1.2m | 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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UKIRT, Gemini and CFHT (Hawaii and Chile) | |||||
| 3.8m UKIRT | |
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WFCAM | |
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| 3.6m CFHT | WFCAM | |
ESPaDOnS | WIRCAM | |
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| Gemini North | GMOS | GMOS | |
NIRI MICHELLE | GNIRS NIFS MICHELLE | |
| Gemini South | GMOS | GMOS | |
T-ReCS | T-ReCS | |
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European Southern Observatory (Paranal, Chile) | |||||
| VLT UT1 | FORS2 | FORS2 | |
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CRIRES |
| VLT UT2 | FORS1 FLAMES / GIRAFFE |
UVES FLAMES / UVES X-SHOOTER |
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X-SHOOTER | |
| VLT UT3 | VIMOS | VIMOS | |
VISIR / ISAAC | VISIR / ISAAC | |
| VLT UT4 | |
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NACO HAWK-I | NACO SINFONI | |
| VISTA | |
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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 | |
| 2.2m MPI | WFI | |
FEROS | |
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South African Astronomical Observatory | |||||
| SALT | SALTICAM | |
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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 | 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 | MOSAIC-II | R-C HYDRA | |
ISPI | |
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| 4.1m SOAR | SOI HTS | HTS | |
OSIRIS | OSIRIS | |
| 1.5m | |
R-C | |
CPAPIR | |
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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 |
|---|---|---|---|
| WHT INT |
~15 September ~15 March |
1 February to 31 July 1 August to 31 January |
UK astronomers have ~40% share (but decreasing) on these telescopes. |
| UKIRT | ~15 August ~15 March |
1 February to 31 July 1 August to 31 January |
It looks like there will be no more calls for proposals. |
| ESO | ~31 March ~29 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. |
| GTC | ~31 March ~30 September |
Large programs only (10+ nights) | The GTC is available through ESO. |
| Gemini | ~2 April ~30 September |
1 August to 31 January 1 February to 31 July |
The UK is (currently) a member of Gemini with full access to the telescopes. This situation should persist until at least semester 2012B. |
| 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. |
| 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. |
| 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 may not apply to SALT, which is restricted to the members of the SALT consortium. |
| 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 |
|---|---|---|---|---|---|---|
| ISIS | Long-slit spectroscopy | Blue: 3500 to 5100 Å Red: 5400 to 10000 Å |
Blue: 0.11 to 1.62 Å/px Red: 0.26 to 1.81 Å/px |
Blue: EEV 4k × 2k CCD Red: REDPLUS 4k × 2k Either arm: an L3CCD with almost zero readout noise is available. |
3.7 arcmin slit length | It has a dichroic, and does observations in the blue and red arms simultaneously |
| WYFFOS | Multi-object spectroscopy | 3700 to 10000 Å | 0.06 to 2.9 Å/px | Mosaic of two EEV 4k × 2k CCDs | 20 arcmin unvignetted | Uses ISIS gratings (or échelle). Up to 150 fibres available. |
| NAOMI/OASIS | Integral-field spectroscopy | 4200 to 9900 Å | 0.37 to 35 Å/px | MIT/LL3 4k × 2k CCD | 3.7 × 2.7 arcsec to 10.3 × 7.4 arcsec | Has 1100 lenslets. Can use the NAOMI adaptive optics system. Used to be at the CFHT. |
| PFIP | Wide-ish field imaging | U B V R I Z (other filters available) |
0.24 arcsec/px | Mosaic of two EEV 4k × 2k CCDs | 16.2 × 16.2 arcmin | Prime focus imaging camera |
| ACAM | Optical imaging | U B V R I Z plus narrow-band filters | 0.25 arcsec/px | AUXCAM (2048 × 4096 EEV CCD) | circular, 8.3 arcmin in diameter | Always mounted except for when the PFIP is in use, so is good for over-rides and ToOs. |
| ACAM | Low-resolution spectroscopy | 3500 to 9000 Å | R ~ 250-900 depending on slit and wavelength | AUXCAM (2048 × 4096 EEV CCD) | 5.8 arcmin long slit | Always mounted except for when the PFIP is in use, so is good for over-rides and ToOs. |
| NAOMI/INGRID | High-resolution IR imaging | 0.8 to 2.5 micron | 0.04 arcsec/px | HgCdTe 1k × 1k array | 40 × 40 arcsec | Uses the NAOMI adaptive optics system |
| LIRIS | IR imaging | 0.8 to 2.5 micron | 0.25 arcsec/px | HgCdTe 1k × 1k array | 4.27 × 4.27 arcmin | |
| LIRIS | Low-resolution IR spectroscopy | 0.8 to 2.5 micron | R = 700 to 2500 | HgCdTe 1k × 1k array | long slits available |
The long-term future of the WHT is not completely secure as its present status is reliant on funding from several Governments, one of which (UK) is becoming increasingly reticent. However, the WHT is an excellent telescope which is also demonstrably cheap to run. It is being steered towards wide-field multi-object spectroscopy, in which case it will be a good survey instrument to support the larger northern telescopes.
| 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 (still being commissioned) |
3.3 arcmin slit width | The 235mm camera is available. The 500mm camera (higher dispersion) is 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. |
The future of the INT is not secure, and depends on the ING being given sufficient funding for its continued low-level operation. At present (2010) the UK government is actively seeking to minise the funding it give to the ING, which is not a good sign for the INT. The telescope is productive but coming towards the end of its economic lifetime.
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| ALFOSC | Grism spectroscopy | 3200 to 11000 Å | R = 190 to 10000 | EEV 2k × 2k | Roughly 5 arcmin | Also has a multi-object spectroscopy mode. Readout time 90s (unbinned) or 32s (2×2). Also does polarimetry. |
| ALFOSC | Optical imaging | 3200 to 9100 Å | 0.19 arcsec/px | EEV 2k × 2k | 5 to 7 arcmin depending on the filter | Also does polarimetry. |
| MOSCA Mosaic Camera |
Optical imaging | UBVRI ugriz uvbyβ | 0.11 arcsec/px | Mosaic of four Loral 2k × 2k CCDs | 7.7 × 7.7 arcmin | Readout time 113s (unbinned) or 37s (2×2 binning). |
| StanCam | Optical imaging | U B V R I | 0.176 arcsec/px | TEK 1k × 1k CCD | 3 × 3 arcmin | Permanently mounted. Also used as slit viewer for FIES. Readout time 43s (unbinned) or 16s (2×2). |
| NOTCAM | IR imaging | 0.8 to 2.5 micron | 0.23 or 0.08 arcsec/px | HgCdTe 1k × 1k array | 4×4 arcmin or 82×82 arcsec | Also does polarimetry. |
| NOTCAM | IR grism spectroscopy | 0.8 to 2.5 micron | R = 2500 or 5500 | HgCdTe 1k × 1k array | Slit length 4 arcmin or 80 arcsec | |
| FIES | Optical échelle spectroscopy | 4000 to 8300 Å | R = 25 000, 45 000 or 65 000 | EEV 2k × 2k CCD | Poor response in the blue due to long fibres. Can do a simultaneous thorium-argon wavelength calibration mode. |
The short-term future of the NOT is stable as the Nordic countries are fully aware of its high capability, reliability and low running costs. The FIES spectrograph is excellent. In the longer term there are indications that it may struggle to attract a high number of applications for observing time, although it would be a valued part of the prospective Common Northern Observatory.
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| SARG | Optical échelle spectroscopy | 3700 to 10000 Å | R = 29 000 to 164 000 | Mosaic of two EEV 4k × 2k CCDs | Long-slit observations can cover up to 30 arcsec | |
| NICS | IR imaging | 0.9 to 2.5 micron | 0.25 to 0.04 arcsec/px | HgCdTe 1k × 1k array | 4.2×4.2 to 0.7×0.7 arcmin | Has two different cameras. Can do polarimetry. |
| NICS | IR grism spectroscopy | 0.9 to 2.5 micron | 2 to 100 Å/px | HgCdTe 1k × 1k array | Can do spectropolarimetry. | |
| LRS / DOLORES | Optical imaging | UBVRI and ugriz plus additional filters |
0.275 arcsec/px | Loral 2k × 2k CCD | 9.4 × 9.4 arcmin | Readout time 20s (unbinned) or 6s (2×2 binning). |
| LRS / DOLORES | Optical low-resolution spectroscopy | 3700 to 10000 Å | R = 300 to 5000 | Loral 2k × 2k CCD | 9.4 arcmin field for MOS. | Can do multi-object spectroscopy. Readout time 20s (unbinned) or 6s (2×2 binning) for full CCD. |
| OIG | Optical imaging | UBVRI and ugriz plus additional filters |
0.072 arcsec/px | Mosaic of two EEV 4k × 2k CCDs | 4.9 × 4.9 arcmin | Readout time 216s (unbinned) or 66s (2×2) or 37s (3×3). |
The future of the TNG must be regarded as uncertain as it is desperately short of money. However, it will benefit from hosting the HARPS-NEF spectrograph, which will soon be commissioned for follow-up of transiting planet candidates discovered by the Kepler satellite.
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| RATCam | Optical imaging | ugriz and BV and Hα | 0.135 arcsec/px | EEV 2k × 2k CCDs | 4.6 × 4.6 arcmin | Readout time 10s (unbinned) or 5s (2×2). 3×3 and 4×4 binning also available. |
| RISE | Optical high-speed imaging | V+R filer (roughly 4600 to 7200 Å) | 0.54 arcsec/px | EEV frame-transfer CCD | 9.2 × 9.2 arcmin | Readout speed is "less than a second". |
| RINGO2 | Optical high-speed polarimetry | V+R filer (4600 to 7200 Å) | 0.45 arcsec/px | E2V electron-multiplying CCD, 512×512 pixels | 3.8 × 3.8 arcmin | Does imaging polarimetry using a rotating polaroid. |
| FRODOspec | Optical medium-resolution spectroscopy | 3900 to 9400 Å | R = 2200 to 5500 | CCDs | 11 × 11 arcsec | Integral-field spectrograph. Has a red and a blue arm which and are capable of obtaining the full optical/near-IR wavelength region in one observation. |
| IO Infrared-Optical imager | Optical/infrared and high-speed imaging | IO:O: ugriz, BV, Hα filters IO:I: JH filters IO:THOR: 5150-9000 Å |
IO:O: 0.15 arcsec/px IO:I: 0.18 arcsec/px IO:THOR: 0.267 arcsec/px |
IO:O: Fairchild 4k × 4k CCD IO:I: 2k × 2k Hawaii HgCdTe array IO:THOR: 1k × 1k EMCCD |
IO:O: 10 × 10 arcmin IO:I: 6 × 6 arcmin IO:THOR: 4.5 × 4.5 arcmin |
Simultaneous optical (IO:O) and infrared (IO:I) imaging is available. IO:THOR is a fast-readout camera which will become available in 2012. |
The future of the telescope is uncertain at this point and it may be funded for only a few more years.
| 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 |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| LAICA | Wide-field optical imaging | 3400 to 10000 Å | 0.225 arcsec/px | Mosaic of four 4k × 4k CCDs | 44.36 × 44.36 arcmin (requires four observations) | CCDs are separated by just under one CCD width in each direction, so four observations are needed to fully cover one field. |
| TWIN | Optical spectroscopy | blue: 3500 to 5000 Å red: 5000 to 10000 Å |
0.36 to 2.2 Å/px | Two SITe 2048×800 CCDs | Slit length up to 4 arcmin | Blue and red arms can operate simultaneously |
| MOSCA | Optical imaging | 3300 to 10000 Å | 0.33 arcsec/px | Normally uses one 4k × 2k CCD | 11 × 11 arcmin | Also does grism and multi-object spectroscopy. |
| MOSCA | Optical grism spectroscopy with MOS capability | 3300 to 10000 Å | 1 to 4 Å resolution | Normally uses one 4k × 2k CCD | 11 × 11 arcmin | Also does imaging and multi-object spectroscopy. |
| 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 |
|---|---|---|---|---|---|---|
| BUSCA | Optical imaging (simultaneous in four bands) | Optical wavelengths | 0.176 arcsec/px | Four 4k × 4k CCDs (the bluemost one thinned) | 12 × 12 arcmin | Dichroics split the light beam with cut-off wavelengths around 4300, 5300 and 7000 Å. Readout time is large (about 2min). |
| AstraLux | Optical "lucky" imaging | 400 to 900 nm | 0.044 arcsec/px | 512 × 512 pixel electron-multiplying CCD | 23 × 23 arcsec !!! | Can run faster than 100 Hz with windowing |
| CAFOS | Optical imaging | 320 to 1100 nm | EEV: 0.53 arcsec/px Loral: 0.33 arcsec/px |
Choice of two 2k × 2k CCDs: EEV (blue-sensitive) or Loral (red-sensitive). | EEV: 16 × 16 arcmin Loral: 10.8 × 10.8 arcmin |
Also does polarimetry and spectroscopy. |
| CAFOS | Optical grism spectroscopy | Optical wavelengths | 2.0 to 9.8 Å/px | Choice of two 2k × 2k CCDs: EEV (blue-sensitive) or Loral (red-sensitive). | EEV: 16 × 16 arcmin Loral: 10.8 × 10.8 arcmin |
Also does imaging and spectropolarimetry and multi-object spectroscopy. |
| 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 |
|---|---|---|---|---|---|---|
| CCD | Optical imaging | BVRI plus other CAHA filters | 0.5 arcsec/px | SITe2b 2k × 2k CCD | 16 × 16 arcmin (BVRI) 11 × 11 arcmin (other CAHA filters) |
Operated remotely. Applications may need to be for large projects requiring many nights. |
The observatory also has a 0.8m Schmidt telescope which is no longer used, and a 1.5m telescope which is operated by a separate group and used only intermittently.
MAGIC is available only at the 2.2m at present, but may become available at the 3.5m and 1.23m as well.
| 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 |
The funding of the OHP is being withdrawn due to structural changes in the French educational system. The 1.93m telescope is currently operating on half the nights and the observatory will likely close in the near future.
| 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 |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| WFCAM | Infrared imaging | 1 to 5 microns | 0.40 arcsec/px | Mosaic of four HgCgTe 2k × 2k arrays cover a quarter of a 53×53 arcmin field in one observation | 40 × 40 arcmin | Four pointing are needed to fully cover each 53×53 arcmin field. |
UKIRT is now running in campaign mode: the UKIDSS survey is being completed as quickly as possible and only the WFCAM instrument is available. From the UKIRT webpage on 17/8/2010: "At this time it is not clear whether a Call for Proposals will be issued for 11A. Please visit the UKIRT homepage in early September for an update." The situation was unchanged on 2011/03/01.
| 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) |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| CRIRES | IR échelle spectroscopy | 0.94 to 5.4 microns | R = 100 000 | Mosaic of four InSb arrays giving total size 4096 × 512 pixels | Slit length is 40 arcsec at 0.086 arcsec/px | Can use the MACAO adaptive optics instrument |
| FORS2 | Optical imaging | Optical, but lowish blue sensitivity | 0.25 or 0.125 arcsec/px | Mosaic of two MIT (red-sensitive) or EEV (blue-sensitive) 2k × 4k CCDs | 6.8 × 6.8 arcmin or 4.25 × 4.25 arcmin | Now has the polarimetry module which was on FORS1. |
| FORS2 | Optical grism spectroscopy | Optical, but lowish blue sensitivity Å | R = 260 to 2600 | Mosaic of two MIT (red-sensitive) or EEV (blue-sensitive) 2k × 4k CCDs | 6.8 × 6.8 arcmin | Also does multi-object spectroscopy. Now has the polarimetry module and some grisms from FORS1. |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| FLAMES / GIRAFFE | Optical multi-object and integral-field spectroscopy | 3700 to 9500 Å | R = 10 000 or 25 000 | EEV 2k × 4k CCD | Deployable IFU allows spectroscopy of 15 objects, each with 20 microlenses (totalling 2×3 arcsec). ARGUS IFU allows spectroscopy of one object using 22×14 microlenses (6.6×4.2 or 11.5×7.3 arcsec). MEDUSA fibres allow 132 spectra to be obtained in one exposure, covering the 25 arcmin field. |
|
| FLAMES / UVES | Optical multi-object échelle spectroscopy | Red optical wavelengths | R = 47 000 | See UVES entry (uses red arm only) | Up to 8 fibres are available per exposure | FLAMES feeds 6 or 8 fibres to the entrance slit of the UVES spectrograph. |
| UVES | Optical échelle spectroscopy | 3000 to 5000 (blue) and 4200 to 11 000 (red) Å | R = 40 000 to 110 000 | Blue arm: EEV 4k × 2k CCD Red arm: Mosaic containing one EEV 4k × 2k CCD and one Loral 4k × 2k CCD |
Long slit maximum is less than 10 arcsec to avoid different orders merging. | Has a blue and a red arm, which can either operated separately or simultaneously using a dichroic. |
| X-SHOOTER | Simultaneous optical-IR échelle spectroscopy | 3000 to 5595 Å (blue) 5595 to 10240 Å (red) 10240 to 24800 Å (IR) |
R = 4500 (blue/IR) R = 7000 (red) |
EEV 4k × 2k CCD (blue), 4k × 2k MIT/LL CCD (red), 2k × 1k Hawaii (IR) | 12 arcsec long slit, plus the option of an image-slicer IFU to improve resolution. | Covers the wavelength range 0.3 to 2.5 μm in ONE exposure using three arms. Optimised for throughput, with a total efficiency of 30% (instrument + telescope + atmosphere). |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| VIMOS | Optical wide-field imaging | U B V R I z | 0.205 arcsec/px | Each arm has one EEV 4k × 2k CCD | Four arms, each with field of view 7×8 arcmin | Also does MOS and IFU spectroscopy. |
| VIMOS | Optical MOS and IFU spectroscopy | 3600 to 10000 Å | R = 200 to 2500 | Each arm has one EEV 4k × 2k CCD | MOS: Four arms, each 7×8 arcmin IFU: 13×13 to 54×54 arcsec. |
Also does imaging. The IFU has 6400 fibres. |
| VISIR | Mid-IR imaging | 8 to 13 micron (N) and 16.5 to 24.5 micron (Q) | N: 0.075 arcsec/px Q: 0.127 arcsec/px |
DRS 256 × 256 BIB detector | N: 19.2 × 19.2 arcsec Q: 32.3 × 32.3 arcsec |
Also does spectroscopy. |
| VISIR | Mid-IR spectroscopy | 8 to 13 micron (N) and 16.5 to 24.5 micron (Q) | R = 350 to 25 000 | DRS 256 × 256 BIB detector | Slit length 32.3 to 4.1 arcsec | Also does imaging. |
| ISAAC | IR imaging | 1 to 5 microns | 0.148 or 0.071 arcsec/px | Choice of two 1k × 1k arrays: HgCdTe (1 to 2.6 micron) or InSb (3 to 5 micron and JHK imaging) | 152×152 or 73×73 arcsec | Will be decommissioned during P90 in favour of SPHERE. Can use the MACAO adaptive optics instrument. |
| ISAAC | IR grating spectroscopy | 1 to 5 microns | R = 500 to 1000 | Choice of two 1k × 1k arrays: HgCdTe (1 to 2.6 micron) or InSb (3 to 5 micron and JHK imaging) | Slit length 120 arcsec | Can use the MACAO adaptive optics instrument |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| SINFONI | IR integral field spectroscopy | 1.1 to 2.45 microns | Spatial: 0.025 or 0.1 or 0.25 arcsec per image slice Spectral: R = 1500 to 4000 |
2k × 2k Hawaii 2RG detector | 8×8 or 3×3 or 0.8×0.8 arcsec | Has adaptive optics. |
| NAOS-CONICA | IR imaging | 1 to 5 microns | 0.0133 to 0.0547 arcsec/px | 1k × 1k Aladin InSb array | 14×14 to 56×56 arcsec | Requires the NAOS adaptive optics. Also does polarimetry. Expected to be decommissioned by the end of 2011 and replaced by MUSE. |
| NAOS-CONICA | IR grism spectroscopy | 1 to 5 microns | R = 400 to 1700 | 1k × 1k Aladin InSb array | 14×14 to 56×56 arcsec | Requires the NAOS adaptive optics. Also does polarimetry. |
| HAWK-I | IR imaging | 0.85 to 2.55 microns | 0.1063 arcsec/px | Mosaic of four Hawaii 2k × 2k detectors | 7.5×7.5 arcmin |
| 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 VST is currently performing multiple public surveys so is only available for guaranteed time observations or for Chilean time.
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.
The future of La Silla Observatory is not assured in the long term, as ESO seeks to shift its funding (which is already focussed on the VLT) to ALMA and construction of an Extremely Large Telescope. There has been a shift towards minimising the number of instruments: the 3.6m has only HARPS and the NTT has only SofI and EFOSC. SofI will be kept running as long as it is technically expedient, so could potentially become ununsable at any time. La Silla will operate until at least 2012. Information on the retired instruments can be found here: SUSI-2, EMMI, TIMMI2 and CES.
Changes from P84 on: visiting astronomers will be assigned a support astronomer but the SA will remain in Santiago rather than being available at the telescopes. A visiting astronomer will still have a telescope operator to operate the telescope.
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| HARPS | Optical échelle spectroscopy | 3780 to 6910 Å | R = 120 000 (standard). Also has wider fibre for higher throughput and lower resolution. | Two EEV 4k × 2k CCDs | Fibre opening is 1 arcsec diameter. | Probably the world's best spectrograph. Simultaneous thorium-argon mode allows wavelength stability of 0.5 m/s. Also does spectropolarimetry. |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| EFOSC | Optical imaging | 3500 to 11000 Å | 0.13 arcsec/px | Loral 2k × 2k CCD | 4.4 × 4.4 arcmin | Also does long-slit and multi-object spectroscopy and polarimetry. |
| EFOSC | Optical grism spectroscopy | 3200 to 11000 Å | 0.92 to 6.66 Å/px plus new VPH grisms with R = 4000 |
Loral 2k × 2k CCD | 4.4 × 4.4 arcmin | Also does imaging and multi-object spectroscopy and polarimetry. |
| SofI | IR imaging | 0.9 to 2.55 microns | 0.144, 0.273 or 0.288 arcsec/px | 1k × 1k Hawaii HgCdTe array | 2.4×2.4 to 4.9×4.9 arcmin | Also does spectroscopy and imaging polarimetry. |
| SofI | IR grism spectroscopy | 0.9 to 2.55 microns | R = 600 to 2200 | 1k × 1k Hawaii HgCdTe array | Also does imaging and imaging polarimetry. |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| WFI | Optical imaging | 3300 to 10000 Å | 0.238 arcsec/px | Mosaic of eight 4k×2k CCDs | 34 × 33 arcmin | Readout time 27s. |
| FEROS | Optical échelle spectroscopy | 3500 to 9200 Å | R = 48 000 | EEV 4k×2k CCD | Fibre entrances subtend 2.0 arcsec | High-efficiency, fixed-format stable instrument. It has two fibres, allowing simultaneous observation of a science target and either a local sky or a ThAr wavelength calibration. |
Only limited time is available on the 2.2m to visiting astronomers, as much of the time is allocated to German and Chilean research. The Max Planck Institute operate the seven-band simultaneous imager GROND, which is not a facility instrument.
Due to the recent funding crisis UK astronomers may soon lose access to the Gemini telescopes (see here). In addition, the Aspen programme of instrument development for Gemini has largely been abandoned for financial reasons. New instruments are currently being worked on (the FLAMINGOS-2 near-IR multi-mode instrument, GSAOI and GPI) and a new longer-term plan is being formulated.
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| GMOS | Optical imaging | 3500 to 11000 Å | 0.073 arcsec/px | Mosaic of three 4k × 2k CCDs | 5.5×5.5 arcmin | Also does long-slit, multi-object or integral-field spectroscopy. The twin instrument on Gemini South has a better blue response. |
| GMOS | Optical spectroscopy | 3500 to 11000 Å | 0.2 to 1.7 Å/px | Mosaic of three 4k × 2k CCDs | IFU has 35×35 arcsec field of view | Does long-slit, multi-object, integral-field spectroscopy. Also does imaging. The twin instrument on Gemini South has a better blue response. |
| NIRI | IR imaging | 1 to 5 microns | 0.022, 0.050 or 0.117 Å/px | Aladin InSb 1k × 1k array | 22×22, 51×51 or 120×120 arcsec | Also does long-slit spectroscopy. Can use the AO system. |
| GNIRS | IR grism spectroscopy | 1 to 5 microns | R = 1700 to 18000 | Aladin InSb 1k × 1k array | Slit width up to 100 arcsec | Can do imaging with its acquisition system. Can do cross-dispersed spectroscopy. |
| NIFS | IR integral-field spectroscopy | 0.95 to 2.40 microns | R = 5000 | Hawaii HgCdTe 1k × 1k array | 3×3 arcsec | Uses the AO system. Can do spectropolarimetry. |
| MICHELLE | Mid-IR imaging | 7 to 26 microns | 0.1005 arcsec/px | IBC Si:As 320 × 240 pixels array | 32×24 arcsec | Uses the AO system. Can do polarimetry. Can also do grating spectroscopy. |
| MICHELLE | Mid-IR grating spectroscopy | 7 to 26 microns | R = 200 to 30 000 | IBC Si:As 320 × 240 pixels array | 0.201 arcsec/px long slit | Uses the AO system. Can also do imaging. |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| GMOS | Optical imaging | 3500 to 11000 Å | 0.073 arcsec/px | Mosaic of three 4k × 2k CCDs | 5.5×5.5 arcmin | Also does long-slit, multi-object or integral-field spectroscopy. The twin instrument on Gemini North has a better red response. Note that fringing in the red is appalling! |
| GMOS | Optical spectroscopy | 3500 to 11000 Å | 0.2 to 1.7 Å/px | Mosaic of three 4k × 2k CCDs | IFU has 35×35 arcsec field of view | Does long-slit, multi-object, integral-field spectroscopy. Also does imaging. The twin instrument on Gemini North has a better red response. Note that fringing in the red is appalling! |
| T-ReCS | IR imaging | 8 to 26 microns | 0.09 Å/px | Raytheon SiAs 320 × 240 pixel array | 28.8×21.6 arcsec | Also does long-slit spectroscopy. Can use the AO system. |
| T-ReCS | IR grism spectroscopy | 8 to 26 microns | Spectral: R = 80 to 1000. Spatial: 0.09 Å/px | Raytheon SiAs 320 × 240 pixel array | Slit length is 21.6 arcsec | Also does imaging. Can use the AO system. |
| 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 |
|---|---|---|---|---|---|---|
| MOSAIC II | Optical wide-field imaging | 3400 to 10000 Å | 0.27 arcsec/px | Mosaic of eight SITe 4k × 2k CCDs | 36 × 36 arcmin | Read-out time 2.5 min using 8-channel read mode. |
| R-C spectrograph | Optical grating spectroscopy | 3500 to 11000 Å | 0.48 to 3.75 Å/px | Loral 3k × 1k CCD | 328 arcsec slit | |
| HYDRA | Optical multi-object spectroscopy | 3500 to 10000 Å | 0.27 to 1.24 Å/px | SITe 4k × 2k CCD | 40 × 40 arcmin | Also has a higher-resolution échelle grating available. |
| ISPI | IR imaging | 1 to 2.5 microns | 0.3 arcsec/px | Hawaii HgCdTe 2k × 2k pixel array | 10.5 × 10.5 arcmin |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| SOI | Optical imaging | 3100 to 10500 Å | 0.077 arcsec/px | Mosaic of two EEV 4k × 2k CCDs | 5.25 × 5.25 arcmin | |
| Goodman HTS | Optical imaging | 3200 to 8500 Å | 0.15 arcsec/px | Mosaic of two UL/LL 4k × 2k CCDs | 5 × 5 arcmin | |
| Goodman HTS | Optical grating spectroscopy | R = 1400 to 6000 | 0.15 arcsec/px | Mosaic of two UL/LL 4k × 2k CCDs | 5 × 2.5 arcmin | Can do multi-object spectroscopy. |
| OSIRIS | IR imaging | 1 to 2.2 microns | 0.32 or 0.13 arcsec/px | Hawaii HgCdTe 1k × 1k pixel array | 3.3×3.3 or 1.3×1.3 arcmin | |
| OSIRIS | IR spectroscopy | 1 to 2.2 microns | R = 1400 to 3000 | Hawaii HgCdTe 1k × 1k pixel array | 3.3×3.3 arcmin | Can do multi-object spectroscopy. |
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| RC spectrograph | Optical grating spectroscopy | 3500 to 9000 Å | resolution 2.2 to 17.2 Å | Loral 1200 × 800 CCD | ||
| CPAPIR | IR wide-field imaging | 1.0 to 2.5 micron | 1.03 arcsec/px | Hawaii HgCdTe 2k × 2k array | 35 × 35 arcmin |
| 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. |
SALT has only recently been constructed. The Robert Stobie Spectrograph will soon be available for imaging, spectroscopy, and multi-object spectroscopy, and has been designed to have a good UV-blue performance. The High Resolution Spectrograph (HRS) is in preparation.
| Instrument | Mode | Wavelength coverage | Resolution | Detector | Field of view | Details |
|---|---|---|---|---|---|---|
| GratingSpec | Optical grating spectroscopy | 3500 to 10000 Å | 0.3 to 3.2 Å/px gives 0.5 to 5.0 Å resolution | SiTE 266 × 1798 CCD | 24 arcsec slit | |
| GIRAFFE | Optical échelle spectroscopy | 4000 to 10000 Å | R = 39 000 | TEK 1k × 1k CCD (cosmetic defects) | (fibre-fed) | Observations can be taken of the blue or red optical wavelength regions (but not simultaneously). A second fibre is available for simultaneous arc or sky spectra, but these options are normally not used. |
| CCD camera | Optical imaging | Optical wavelengths | 0.12 arcsec/px | TEK 1k × 1k CCD | 2.5×2.5 arcmin | Also used on 1m telescope. |
| UCT CCD | Optical imaging | Optical wavelengths | 0.13 arcsec/px | EEV 576 × 420 CCD | 1.2×0.9 arcmin | Has high-speed frame transfer capability. Can also be used on 1m and 0.75m telescopes. |
| 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. | Can observe 392 objects simultaneously. Can also do integral-field spectroscopy (512 fibres covering 22×11 arcsec). |
| IRIS2 | IR imaging | 0.9 to 2.5 microns | 0.45 arcsec/px | HgCdTe 1k × 1k array | 7 × 7 arcmin | Also does imaging. Can use the AO system. |
| IRIS2 | IR grism spectroscopy | 0.9 to 2.5 microns | R = 2400 | HgCdTe 1k × 1k array | 7 × 7 arcmin | Does multi-object or long-slit spectroscopy. |
| UCLES | Optical échelle spectroscopy | Optical wavelengths | R = 40 000 to 120 000 | Choice of EEV 4k × 2k CCD (blue-sensitive) or MIT-LL 4k × 2k CCD (red-sensitive) | Choice of two dispersive gratings. | |
| UHRF | Optical échelle spectroscopy | Optical wavelengths | R = 300 000, 600 000 or 940 000 | EEV 4k × 2k CCD | Wavelength coverage 4 to 45 Å | Red-sensitive MIT-LL CCD is available but its lack of binning means it is not as suitable as the EEV chip (which is normally binned 8×8 for the UHRF). |
