3D meeting Tenerife July 2002 Ian Parry, Andrew Dean, Dave King, Andy Bunker, Steve Medlen, Jim...
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Transcript of 3D meeting Tenerife July 2002 Ian Parry, Andrew Dean, Dave King, Andy Bunker, Steve Medlen, Jim...
3D meeting Tenerife July 2002
Ian Parry, Andrew Dean, Dave King, Andy Bunker, Steve Medlen, Jim Pritchard, Rachel Johnson, Anamparabu Ramaprakash,
Rob Sharp, Richard McMahon, Craig Mackay,Gerry Gilmore, Douglas Gough,
Talk given by Andy Bunker on behalf of Ian Parry, Euro3D meeting 02 July 2002
3D meeting Tenerife July 2002
GEMINI-SOUTH
3D meeting Tenerife July 2002
CIRPASS willgo here
GEMINI-SOUTH
3D meeting Tenerife July 2002
· 490 spatial samples and several image scale options (fibre-fed)
· Operation in the range 0.85-1.8mm· Limiting magnitudes of J~21.9 and H~20.9
in 3 hours on Gemini· Limiting flux ~2e-18 ergs/sec/cm^2· Large wavelength coverage (Dl=0.44mm) at
R~3100 in a single integration with a 2048 array
· Spectral resolutions up to R~26,000
Integral Field Spectroscopy
3D meeting Tenerife July 2002
Current Performance Using a 1024x1024 Hawaii-I array and an 8-inch
telescope End to end throughput (J & H) ~6-8% Intrinsic detector dark current is 0.03 e/sec/pix Instrument backgrounds (e/s/pix):
0.15 (J), 0.17 (H-short), ~2 (H-long) Readnoise 17 e rms per read Sky-sky noise lim flux of 2e-18 ergs cm-2 sec-1 in 3
hours on an 8-m telescope Line FWHM 1.4 pixels = 3.1 Angstroms (400 l/mm)
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
Star formation history 1<z<2rotation curves of z~1 galaxiesDamped Lyman-alpha systemsGravitational lensesQSO environmentsULIRGSAlignment effectLINERs
Galactic centreCentres of globular clustersBrown DwarfsStar formation regionsSolar system - Kuiper belt, SatellitesCataclysmic variables
CIRPASSSCIENCE
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
CIRPASS - FOREOPTICS
SPIRAL conceptChanging scale or telescope only involves
changing the magnifying lens
3D meeting Tenerife July 2002
Image Scales Using the CIRPASS IFUon the VLT or Gemini 8-m
Sampling scale FOV(arcsec/lens) (arcsec)
0.33 12.2x5.00.25 9.3x3.50.12 4.4x1.7
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
Suppression Masks (1998)
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
CIRPASSFILTERWHEEL
3D meeting Tenerife July 2002
Observing sequence
Read array very 1-5 minutes (CR rejection and readnoise reduction)
Beam switch so that each fibre spends half the time on object and half the time on sky: ABBAABBA sequence
Dither so that each spatial sample on object is measured using at least 8 different areas on the array
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
Data reduction software
Pipeline controlled by fits headers Runs in real-time under IRAF Supports Euro 3D data format standard
(Euro-network starts July 2002) Sky subtraction, flat-fielding, CR rejection,
spectral extraction, 2d continuum, line and velocity maps, wavelength calibration, flux calibration, etc.
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
SKY-DARK3600slong J
3D meeting Tenerife July 2002
SKY-DARK3600sshort H
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
3D meeting Tenerife July 2002
CIRPASS
Raw Beam-switched(sky-subtracted)
3D meeting Tenerife July 2002
CIRPASS
Sky minus sky, 3 hours, ~500 counts inline gives 2e-18 ergs/sec/cm^2 flux on 8m
3D meeting Tenerife July 2002
H=6.11, KO V star, 15 mins
Cambridge Water
3D meeting Tenerife July 2002
Further improvements to S/N Look at a darker sky Use a bigger telescope Alternative 1024 array and new 2048 array
have higher QE, etc. Reduce effective read-noise by using more
NDRs A new 1.8mm shortpass filter will give an
instrument background of ~0.05 e/s/pix Use optimally designed suppression masks
3D meeting Tenerife July 2002
CIRPASS was shipped to Gemini-S mid-June 2-3 week test programme using our small test
telescope at Cerro Pachon 5 night Science Demonstration run in early Aug
on Gemini-S 8 night MOS run on the AAT in Oct
Schedule
3D meeting Tenerife July 2002
CIRPASS worked very well in Cambridge and we are ready to begin a campaign of scientific exploitation on major telescopes
IFU is easily interfaced to various telescope focii including AO feeds - smaller telescopes give wider FOV
IFU is better than a slit for conventional long-slit targets
Very sensitive - reaches very faint limits Very versatile NIR spectrograph - IFU, MOS,
3000<R<26000
Conclusions