1. 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

2. 3D meeting Tenerife July 2002 GEMINI-SOUTH

3. 3D meeting Tenerife July 2002 CIRPASS will go here GEMINI-SOUTH

4. 3D meeting Tenerife July 2002  490 spatial samples and several image scale options (fibre-fed)  Operation in the range 0.85-1.8  m  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 (  =0.44  m) at R~3100 in a single integration with a 2048 array  Spectral resolutions up to R~26,000 Integral Field Spectroscopy

5. 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 0 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)

6. 3D meeting Tenerife July 2002

7. Star formation history 1<z<2 rotation curves of z~1 galaxies Damped Lyman-alpha systems Gravitational lenses QSO environments ULIRGS Alignment effect LINERs Galactic centre Centres of globular clusters Brown Dwarfs Star formation regions Solar system - Kuiper belt, Satellites Cataclysmic variables CIRPASS SCIENCE

8. 3D meeting Tenerife July 2002

9. CIRPASS - FOREOPTICS SPIRAL concept Changing scale or telescope only involves changing the magnifying lens

10. 3D meeting Tenerife July 2002 Image Scales Using the CIRPASS IFU on the VLT or Gemini 8-m Sampling scaleFOV (arcsec/lens)(arcsec) 0.3312.2x5.0 0.259.3x3.5 0.124.4x1.7

11. 3D meeting Tenerife July 2002

20. Suppression Masks (1998)

21. 3D meeting Tenerife July 2002

24. CIRPASS FILTER WHEEL

25. 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

26. 3D meeting Tenerife July 2002

27. 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.

28. 3D meeting Tenerife July 2002

29. SKY-DARK 3600s long J

30. 3D meeting Tenerife July 2002 SKY-DARK 3600s short H

31. 3D meeting Tenerife July 2002

33. CIRPASS Raw Beam-switched (sky-subtracted)

34. 3D meeting Tenerife July 2002 CIRPASS Sky minus sky, 3 hours, ~500 counts in line gives 2e-18 ergs/sec/cm^2 flux on 8m

35. 3D meeting Tenerife July 2002 H=6.11, KO V star, 15 mins Cambridge Water

36. 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 1.8  m shortpass filter will give an instrument background of ~0.05 e/s/pix • Use optimally designed suppression masks

37. 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

38. 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