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

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

Overview of capabilities
Application eligibility and deadlines
Details for each telescope and instrument
Date of last modification: 05/09/2010

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

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

Overview of capabilities

	Optical imaging
	Optical spectroscopy
	Optical échelle spectroscopy
	Infrared imaging
	Infrared spectroscopy
	Infrared échelle spectroscopy

	Optical wavelengths			Infrared wavelengths
	Imaging	Spectroscopy	Échelle spec.	Imaging	Spectroscopy	Échelle spec.
	La Palma (Spain)
WHT 4.2m	PFIP ACAM	ISIS WYFFOS OASIS ACAM		INGRID LIRIS	LIRIS
INT 2.5m	WFC	IDS
NOT 2.5m	ALFOSC MOSCA StanCam	ALFOSC	FIES	NOTCAM	NOTCAM
TNG 3.6m	DOLORES OIC	DOLORES	SARG	NICS	NICS
LT 2.0m	RATCam RISE	FRODOspec
GTC 10.4m	OSIRIS	OSIRIS		CanariCam	CanariCam
	Calar Alto (Spain)
3.5m	LAICA MOSCA	MOSCA PMAS TWIN		Omega-2000 Omega-Cass
2.2m	BUSCA CAFOS AstraLux	CAFOS		MAGIC	MAGIC
1.2m	CCD
	UK Infrared Telescope (Hawaii)
3.8m UKIRT				WFCAM
	Gemini (Hawaii and Chile)
Gemini North	GMOS	GMOS		NIRI MICHELLE	NIRI NIFS MICHELLE
Gemini South	GMOS	GMOS		T-ReCS	T-ReCS
	European Southern Observatory (Paranal, Chile)
VLT UT1	FORS2	FORS2				CRIRES
VLT UT2		FORS1 FLAMES / GIRAFFE	UVES FLAMES / UVES X-SHOOTER			X-SHOOTER
VLT UT3	VIMOS	VIMOS		VISIR / ISAAC	VISIR / ISAAC
VLT UT4				NACO HAWK-I	NACO SINFONI
VISTA				OmegaCAM
	European Southern Observatory (La Silla, Chile)
3.6m			HARPS
NTT 3.6m	EFOSC	EFOSC		SofI	SofI
2.2m MPI	WFI		FEROS
	Las Campanas Observatory (Chile)
Magellan Baade	IMACS	IMACS		PANIC	FIRE
Magellan Clay	MagIC	MagE	MIKE
2.5m du Pont	CCD WFCCD	B & C	Échelle	WIRC
1.0m Swope	CCD			RETROCAM
	Kitt Peak National Observatory (Arizona, USA)
4m Mayall	MOSAIC	R-C MARS	Échelle	NEWFIRM SQIID FLAMINGOS	FLAMINGOS IRMOS
2.1m	CCD	GoldCam		SQIID FLAMINGOS	FLAMINGOS
WIYN 3.5m	MIMO OPTIC	Hydra		WHIRC
WIYN 0.9m	MOSAIC
	Cerro Tololo Inter-American Observatory (Chile)
4m Blanco	MOSAIC-II	R-C HYDRA		ISPI
4.1m SOAR	SOI HTS	HTS		OSIRIS	OSIRIS
1.5m		R-C		CPAPIR
1.3m	ANDICAM			ANDICAM
1.0m	Y4KCAM
0.9m	CCD
	South African Astronomical Observatory
SALT	SALTICAM
1.9m Radcliffe	CCD camera UCT CCD	GratingSpec	GIRAFFE
1.0m	CCD camera UCT CCD
	Anglo-Australian Observatory (Siding Springs, Australia)
4.0m AAT		AAOmega	UCLES UHRF	IRIS2	IRIS2

	Imaging	Spectroscopy	Échelle spec.	Imaging	Spectroscopy	Échelle spec.
	Optical wavelengths			Infrared wavelengths

Telescope availability and applying for time

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

Telescopes	Deadlines	Semesters	Notes
WHT INT	~15 September ~15 March	1 February to 31 July 1 August to 31 January	UK astronomers have ~40% share (but decreasing) on these telescopes.
UKIRT	~15 August ~15 March	1 February to 31 July 1 August to 31 January	UKIRT is now run in campaign mode, but a small proportion of its time is available for applciations in the usual way through PATT. The UK now conducting a phased withdrawal from UKIRT. There may be no more calls for proposals.
ESO	~31 March ~30 September	1 October to 31 March 1 April to 30 September	The UK is a member of ESO so can apply for all ESO telescopes.
Gemini	~2 April ~30 September	1 August to 31 January 1 February to 31 July	The UK is (currently) a member of Gemini with full access to the telescopes. This situation is not expected to last for a long time.
LT	~15 September ~15 March	1 February to 31 July 1 August to 31 January	UK astronomers have a share on this telescope through PATT.
AAT	~1 September ~1 March	1 February to 31 July 1 August to 31 January	UK astronomers can apply via OPTICON.
NOT	~1 September ~1 March	1 October to 31 March 1 April to 31 September	UK astronomers can apply via OPTICON.
TNG	~1 September ~1 March	1 August to 31 January 1 February to 30 July	UK astronomers can apply via OPTICON.
Calar Alto	~1 September ~1 March	1 July to 31 December 1 Jan to 30 June	UK astronomers can apply via OPTICON.
LCO			Available only through Carnegie, a few other US institutions, or Chilean time.
CTIO	31 March 30 September	August to January February to July	Available through NOAO. Non-US astronomers must justify why they need to use US facilities (i.e. why they cannot use other facilities which are available to them).
KPNO	31 March 30 September	August to January February to July	Available through NOAO. Non-US astronomers must justify why they need to use US facilities (i.e. why they cannot use other facilities which are available to them).
SAAO	1 October 18 December 1 April 1 July	January to March April to June July to September October to December	A "certain percentage" of time goes to astronomers of any nationality. This may not apply to SALT, which is restricted to the members of the SALT consortium.
GTC	~31 March ~30 September	Large programs only (10+ nights)	The GTC was for a while available through ESO, but no new applications will be accepted.

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

Basic details of telescopes and instruments

	Optical imaging
	Optical spectroscopy
	Optical échelle spectroscopy
	Infrared imaging
	Infrared spectroscopy
	Infrared échelle spectroscopy

La Palma

Isaac Newton Group (ING)

4.2m William Herschel Telescope (WHT)

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

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

2.5m Isaac Newton Telescope (INT)

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

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

2.5m Nordic Optical Telescope (NOT)

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

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

3.6m Telescopio Nazionale Galileo (TNG)

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

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

2.0m robotic Liverpool Telescope (LT)

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

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

10.4m Gran Telescopio Canarias (GTC)

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

Calar Alto

3.5m telescope

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

Omega-Cass is currently only available for imaging.

2.2m telescope

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

1.23m telescope

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

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

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

3.8m United Kingdom Infrared Telescope (UKIRT)

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

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

European Southern Observatory (ESO)

Paranal observatory (VLT)

8.2m VLT Unit Telescope 1 (Antu)

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

8.2m VLT Unit Telescope 2 (Kueyen)

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

8.2m VLT Unit Telescope 3 (Melipal)

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

8.2m VLT Unit Telescope 4 (Yepun)

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

4m VISTA Visible and Infrared Survey Telescope for Astronomy

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

Other facilities at Paranal

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

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

La Silla Observatory

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

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

3.6m telescope

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

3.6m New Technology Telescope (NTT)

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

2.2m MPI telescope

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

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

Las Campanas Observatory (LCO)

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

6.5m Magellan Baade telescope

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

6.5m Magellan Clay telescope

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

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

2.5m Irénée du Pont telescope

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

1.0m Henrietta Swope telescope

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

Gemini Observatory

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

8.1m Gemini North (Mauna Kea, Hawaii)

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

8.1m Gemini South (Cerro Pachon, Chile)

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

Kitt Peak National Observatory (KPNO)

4m Mayall telescope

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

2.1m telescope

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

3.5m WIYN telescope

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

0.9m WIYN telescope

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

Cerro Tololo Inter-American Observatory (CTIO)

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

4m Blanco telescope (Cerro Tololo)

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

4.1m SOAR telescope (Cerro Pachon)

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

1.5m telescope (Cerro Tololo)

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

1.3m telescope (Cerro Tololo)

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

1.0m telescope (Cerro Tololo)

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

0.9m telescope (Cerro Tololo)

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

South African Astronomical Observatory (SAAO)

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

11m Southern African Large Telescope (SALT)

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

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

1.9m Radcliffe Telescope

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

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

1.0m telescope

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

Anglo Australian Observatory (AAO) (Siding Springs)

3.9m Anglo Australian Telescope (AAT)

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