Optical telescopes available to UK astronomers (May 2006)
La Palma
========
ING WHT 4.2m ISIS: low-medium resolution double-arm grating spectrograph
Blue arm: dispersions 0.11-1.62 A/px, range 3500-5100 A
Red arm: dispersions 0.23-1.63 A/px, range 5500-9000 A
AF2/WYFFOS: multi-object low-resolution spectrograph
maximum 150 fibres, distributed over 25 arcmin field
NAOMI/INGRID: IR imaging (40 arcsec! field)
NAOMI/OASIS: IR integral-field spectroscopy
LIRIS: IR imaging and low-resolution spectroscopy (4 arcmin field)
PFI: prime focus optical imaging with two 2048x4096 mosaiced CCDs
(16 arcmin field at 0.24"/px)
Aux port: optical imaging with 1024x1024 CCD, mounted when the PFI is
not available (e.g., with ISIS). 1.8 arcmin field at 0.11"/px.
INT 2.5m WFC: four mosaiced 4096x2048 CCDs have 34.2 arcmin field at 0.33"/px
IDS: low-medium resolution grating spectrograph
** Only the 235mm camera is available at present **
235mm camera: dispersion 0.24-3.7 A/px, coverage 536-8000 A
500mm camera: dispersion 0.10-0.8 A/px, coverage 245-4000 A
NOT 2.5m ALFOSC: optical faint-object imaging, spectroscopy, MOS, polarimetry
imaging: 5-7 arcmin field depending on filter
spectroscopy: grisms give 0.65-36 A resolution (2 pixel, 0.5" slit)
echelle spectroscopy: double grisms used (medium resolution)
MOSCA: four 4096x2048 CCD mosaic (7.7 arcmin field at 0.2"/px binned x2)
NOTCam: NIR imaging, spectroscopy, polarimetry (commissioned early 2006)
imaging: 4' fov at 0.2 AA/px or 1.4' fov at 0.08 AA/px
spectroscopy: grism or long-slit
FIES: high-resolution fibre-fed echelle spectrograph. Maximum resolving
power is 65000. Spectral coverage is 4000-8300 A.
TNG 3.6m SARG: echelle spectrograph (R = 29000-164000)
NICS: NIR imaging (4.2 arcmin field), spectroscopy (R=50-2000), polarimetry
DOLORES: focal reducer imager (9.4 arcmin field) and spectrograph
(R = 300-3000) with MOS capability
OIG: optical imaging with field up to 10 arcmin with two 4096x2048 CCDs
Liverpool RATCam imager: 2048x2048 CCD, 4.6 arcmin field, 0.135"/px, ugrizBV filters
Telescope SupIRCam: IR imaging: 1.7' fov at 0.4 AA/px, JHK' filters available
2.0m FRODOSpec: integral-field spectrograph intended to be available late 2007
Calar Alto
==========
3.5m ALFA: adaptive optics including a laser guide star
LAICA: large area imager with four 4096x4096 CCDs, field 44'x44' at
0.23"/px, read-out 70 sec, Johnson UBVRI and Sloan ugriz filters
MOSCA: multi-purpose focal reducer instrument for imaging, slit spectroscopy
and MOS. Imaging: field 11x11 arcmin at 0.32"/px, UBVRIZ filters.
Slit spectroscopy: seven grisms available for 3000-10000 A giving
between 1 and 4 A/px. MOS: you have to bring your own masks!
OMEGA-2000: prime focus large-field IR imager: 15.4 arcmin field at 0.45"/px
OMEGA-Cass: IR imaging, grism spectroscopy, polarimetry for 1.0-2.5 microns.
OMEGA-Prime: IR imaging, 1.0-2.5 microns, 6.8 arcmin field at 0.4"/px.
PMAS Potsdam Multi Aperture Spectrograph: Cassegrain IFU spectrograph.
Gives 16x16 grid of spectra at 0.35, 0.8 or 1.7 A/px.
TWIN two-channel spectrograph: 2000x800 CCDs, resolutions 0.3 to 2.25 A/px,
12 gratings available, and several beamsplitters.
MAGIC IR imaging camera: 256x256 pixels at 0.81, 0.32, 0.18, 0.08 "/px.
Has been superseded by OMEGA.
2.2m BUSCA simultaneous four-colour imaging: 4096x4096 CCDs with 12 arcmin field
at 0.18"/px (but 2x2 binning used under normal conditions), optimised
for uvbyHbeta and Bessell I filters (u and v are not both usable at
the same time). Readout time is large: about 2 minutes
CAFOS focal reducer does imaging, spectroscopy, MOS, polarimetry. Two CCDs
are available, optimised for blue (SITe) or red (LORAL) wavelengths.
Imaging: 16 arcmin field, 0.53"/px (SITe) or 11 field, 0.33"/px (LORAL).
Spectrscopy: 8 grisms available giving between 2 and 10 A/px.
MOS: you have to bring your own slit masks.
FOCES high-resolution echelle spectrograph. Maximum resolving power 65000
(two pixels), optimal is 40000. Full spectral coverage is 3000 A in
70 orders, usable from 3600 to 9400 A.
MAGIC IR imaging camera: 256x256 pixels at 1.62 or 0.64 "/px.
1.23m MAGIC IR imaging camera: 256x256 pixels at 1.2"/px.
European Southern Obervatory, Chile
===================================
La Silla 2.2m WFI Wide Field Imager: 2 4Kx2K CCD mosaic, 33' fov at 0.24"/px
FEROS: fibre echelle spectrograph: resolving power = 48000, coverage
3500-9200 A each observation, setup is fixed.
GROND Gamma-Ray Burst Optical/Near-Infrared Detector: available 2007.
3.6m HARPS fibre echelle spectrograph intended for RV searchs for planets:
resolving power = 120000, coverage each exposure 3780--6901 A.
Second fibre available for simultaneous arc lamp or sky spectra.
EFOSC2: imaging, low-res spectroscopy, spectropolarimetry and MOS
imaging: 5.2arcmin field at 0.157"/px with 20948x2048 CCD
spectroscopy: resolution is 5.9-41 AA (6 px!) depending on grism
TIMMI2: multi-mode instrument for the IR (3-25 um) ** RETIRED **
CES: Coude Echelle Spectrograph (very high resolution) ** RETIRED **
NTT 3.6m EMMI: ESO Multi-Mode Instrument (has a blue and a red arm)
blue arm: CCD is 1024x1024 Tektronix
red arm: two mosaiced MIT/LL CCDs, each 2048x4096
wide-field imaging: 6.2 arcmin field (blue), 9.1x9.9 (red)
high-resolution imaging: 2.2 arcmin field at 0.13"/px
low-resolution spectroscopy: resolving power 280-1670 depending
on grating (and multi-object capability)
medium-dispersion spectroscopy: resolving power 840-9000 in the
blue arm and 600-70000 in the red arm
echelle spectroscopy: resolving power 7700-70000
SOFI: NIR (0.9-2.5 um) imaging (4.9arcmin field) and low-resolution
spectroscopy (resolving power 600-2200)
SUSI2: high-res imaging over 5.5 arcmin field at 0.08"/px.
Has two 4096x2048 CCDs mosaiced together.
Paranal VLT UT1 CRIRES: high-res IR longslit spectrograph (newly commissioned), 1-5
um sensitivity, R=100000 with 0.2" slit, 1024x1024 CCD mosaic
FORS2: two 4096x2048 CCDs for imaging (6.8 arcmin field), spectroscopy
(resolving power 260-2600 depending on grism), MOS (up to 19
slitlets), or high-speed spectroscopy (HIT mode).
ISAAC: IR (1-5 um) imaging (2.5 arcmin field), spectroscopy (R=500-3000)
VLT UT2 FORS1: similar to FORS2 but with one 2048x2048 CCD: less sensitive in
the red, more sensitive in the blue. Imaging: 6.8 arcmin field.
Spectroscopy: R=260-1700 dep on grism. It can also do polarimetry
FLAMES: multi-object fibre feed to the GIRAFFE or UVES spectrographs
to GIRAFFE: up to 132 objects for R=5600-46000 grating spectroscopy
to GIRAFFE: IFU with field of view up to 11.5x7.3 arcmin
to UVES: 8 fibres and R=47000 with 2000 A range each exposure
UVES: high-resolution cross-dispersed echelle spectrograph with red and
blue arms (sensitive between 3000 AA and 1.1 um). R=4000 with 1"
slit, but can achieve R=80000 in the blue arm and R=11000 in the
red arm. Iodine cell is avaiable for high-accuracy RV studies.
VLT UT3 VISIR: mid-IR (8-24 um) imaging (19" or 32" field!) and grating or
echelle spectroscopy (R=320, 3200 or 25000)
VIMOS: optical wide-field imaging (7'x8' fov) and MOS (R=200-2500
dep on grism) with an IFU capability. There are four separate
arms, so imaging may be conducted over more than 7'x8'?
VLT UT4 SINFONI: near-IR IFU spectroscopy (R=1500-4000) with adaptive optics
NACO=NAOS/CONICA: near-IR (1-5 um) adaptive optics assisted imaging,
imaging polarimetry, coronography and spectroscop, 1024x1024 CCD
Gemini
======
Gemini North Altair: facility adaptive optics imstrument for use with other ones
GMOS: Gemini Multi-Object Spectrograph. 0.36-1.10 um long-slit and
multi-object spectroscopy and imaging over a 5.5 arcmin field.
Detector: three 2048x4608 CCDs give 0.073" pixels!
Six gratings give 0.2-1.7 A/px with coverage 1430-10000 A!
Also does integral field spectroscopy over 35"x35".
Michelle: mid-IR (7-26 um) imaging and long-slit spectroscopy
Detector: 320x240 px SiAs array. Imaging: 0.1"/px gives field
32"x24". Spectroscopy: resolving powers of 110 to 30000.
NIFS: Near-infrared Integral Field Spectrometer.
NIRI: Near-IR (1.0-5.5 um) imager and grism spectrograph. 1024x1024
InSb detector array with three cameras giving 0.022, 0.050,
and 0.117"/px (fields 22, 51, and 120 arcsec).
TEXES: high resolution (R~100000) mid-IR (5-25 um) spectrometer
Gemini South GMOS: Gemini Multi-Object Spectrograph. 0.36-1.10 um long-slit and
multi-object spectroscopy and imaging over a 5.5 arcmin field.
Detector: three 2048x4608 CCDs give 0.073" pixels!
Six gratings give 0.2-1.7 A/px with coverage 1430-10000 A!
Also does integral field spectroscopy over 35"x35".
bhROS: high resolution optical spectrograph. Optical fibres feed a
cross-dipersed echelle giving resolving power 150,000.
** INDEFINITELY REMOVED FROM USE IN 2007 **
Acquisition Camera: can be used for high-speed photometry. CCD is a
1024x1024 frame-transfer with no shutter (2.2 arcmin field).
Phoenix: high-resolution near-IR (1-5 um) spectrograph. Resolving
powers of 50000 to 75000. Detector is 1024x1024 InSb device.
GNIRS: near-IR (1-5.5 um) spectrograph, operable in long-slit, cross-
dispersed and integral-field modes. Resolving power 1700-18000.
T-ReCS: mid-IR (8-26 um) imager and long-slit spectrograph. Detector
is 320x240 px SiAs array. Imaging: 0.09"/px gives 28.8x21.6
arcsec field. Spectroscopy: resolving powers 100 to 1000.
South Africa
============
1.9m Radcliffe grating spectrograph: resolution 0.5-3 A, range 350-3200 A
GIRAFFE: fibre echelle spectrograph, R=39000, sensitivity 3820-9240 A but obs
only in blue or red simultaneously. Second fibre for sky or arc spectrum.
CCD imaging: 1024x1024 CCD (is oversampled) gives 2.5 arcmin field at 0.14"/px.
UCT frame transfer CCD: 576x420 px gives 1.2x0.9 arcmin field at 0.13"/px
1.0m Elizabeth CCD imaging: 1Kx1K CCD gives 5 arcmin field at 0.31"/px
UCT frame transfer CCD: 576x420 px gives 2.7x2.0 arcmin field at 0.30"/px
Australia
=========
AAT 4.0m UHRF: ultra high resolution echelle spectrograph with R=300000,600000,940000
and spectrum length 4-45 AA depending on resolving power and wavelength
UCLES: echelle spectrograph with R=40000 (1" slit) to R=100000. Good wavelength
coverage possible, and an iodine cell for high-accuracy RV studies
IRIS2: IR (0.9-2.5 um) imaging (7.7' fov), longslit spectroscopy (R~2400) or
multi-object spectroscopy (up to 40 objects)
AAOMEGA/2dF: multi-object spectrograph for 350-400 objects at R=2000-13000
(tbc). 2dF fibre feed has 2 degree fov. IFU spectroscopy possible too.
WFI Wide Field Imager: Mosaic of eight 4096x2048K CCDs gives 33 arcmin field
at 0.22 AA/px. ** NO LONGER AVAILABLE AS COMMON-USER INSTRUMENT **
ATT 2.3m Imager: 6 arcmin diameter circular field at 0.3"/px. Image quality ~2".
DBS Double Beam Spectrograph: blue and red arms with dichroic beamsplitter.
Resolution 0.5-4.5 A (blue arm) or 1.1-8.1 A (red arm)
CASPIR: IR spectrograph
Applying for time
=================
PATT telescopes: Apply 15 Sept for 1 Feb to 31 July
(WHT, INT, AAT) Apply 15 March for 1 Aug to 31 Jan
NOT: Available to all but a Nordic PI is helpful.
1st working day of May for 1 Oct to 31 Mar
1st working day of Nov for 1 Apr to 30 Sep
TNG: no financial support for non-INAF astronomers,
but a time-share with PATT is set up
Calar Alto: 2006 deadlines are 15 March (for 1 July to 31 Dec) and 15 Sept
(for 1 Jan to 30 June). No restriction on who may apply.
ESO telescopes: Apply ~31 March for semester 1 Oct to 31 Mar
Apply ~30 Sept for semester 1 April to 30 Sept
Gemini: semester 2007B (01/08/2007 to 31/01/2008) deadline 02/04/2007
SAAO telescopes: Apply 1 Oct for January to March
Apply 18 Dec for April to June
Apply 1 April for July to September
Apply 1 July for October to December
ATT: any Australian or overseas astronomer may apply for RSAA telescopes
Apply 15 Feb for May to July Apply 15 May for Aug to Oct
Apply 15 Aug for Nov to Jan Apply 15 Nov for Feb to April
LT: Deadlines in March and Sept for the same? semesters as PATT.
Complication concern which type of observing to go for, as
everything happens automatically in robotic queue mode.