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