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Gemini Observatory Results & Lessons Leaned

Gemini Observatory Results & Lessons Leaned. SPIE August 2002 Matt Mountain Jean-Rene Roy Phil Puxley Eric Hansen. Defining Gemini: Top Level Performance Requirements – (1991 SRD). Image Quality of better than 0.1 arcsec. < 2.5 m m Diffraction limited imaging with Adaptive Optics

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Gemini Observatory Results & Lessons Leaned

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  1. Gemini ObservatoryResults & Lessons Leaned SPIE August 2002 Matt Mountain Jean-Rene Roy Phil Puxley Eric Hansen

  2. Defining Gemini:Top Level Performance Requirements– (1991 SRD) • Image Quality of better than 0.1 arcsec. < 2.5 mm • Diffraction limited imaging with Adaptive Optics • IR Optimized configuration • Board wavelength coverage and high throughput • Versatility • Exploit Queue Scheduling

  3. Potter et al 2001 Potter et al 2001 Close et al 2001 Potter et al 2001 Jayawardhana & Luhman, 2002 Liu et al 2001 Early AO Science Results Trapezium, J,H & K Gemini South (Lucas 2002)

  4. Flux (photons/sec/µm/arcsec2 ) OH Wavelength (µm) IR Optimization – energy concentration & low emissivity

  5. IR Optimization works:Gemini-South IR (4 micron) Commissioning Images of Galactic Center • Simons & Becklin 1992 • IRTF (3.6m) - L’ • 16,000 images shift/add • An entire night…. • Gemini South + ABU + fast tip/tilt • Brackett  • FWHM ~ 0.35” • 1 minute integration

  6. 14 mJy/pixel after further IR Optimization Gemini North: M87 jet at 10 mm– Deepest image ever taken in the mid IR Perlman, Sparks, et al. HST/F300W, 0.3 m OSCIR, 10.8 m • Sensitivity (1, 1 h): 0.028 mJy/pix (pix scale = 0.089”) 0.1 mJy on point source

  7. Mauna Kea, Hawaii The Frederick C. Gillett Gemini Telescope

  8. Gemini in the Optical – GMOS North comes on-line 60min – 140min per filter Seeing (FWHM) 0.5 – 0.7 arcsec 5 sigma detection limits : g'=27.5 mag r'=27.2 mag i'=26.3 mag GMOS on Gemini 5.5’ x 5.5’ PMN2314+0201 Quasar at z=4.11 Gemini SV PI: Isobel Hook

  9. GMOS Queue Observing 2002A Summary of the completion rates as fraction of programs ========================================================== Band Completion rate >90% >50% <50% ----------------------------------------- 1 10/14=0.71 11/14=0.79 3/14=0.21 2 2/8 =0.25 3/8 =0.38 5/8 =0.63 3 2/8 =0.25 4/8 =0.50 4/8 =0.50 4 1/11=0.09 2/11 =0.18 9/11=0.82 Many observations in band 3 and 4 were taken in poor observing conditions, and the programs in these bands with significant data were programs that could tolerate CC=70% or worse, and seeing of 1arcsec or worse. Gemini North reliability >90% (<10% down time) GMOS Observing efficiency (shutter open/elapsed) ~ 70%

  10. GMOS: Evolution of ages and metalicity in clusters from z= 1 to present epoch (Inger Jørgensen , Gemini Observatory) Abel 851 z = 0.4

  11. GMOS: Evolution of ages and metalicity in clusters from z= 1 to present epoch (Inger Jørgensen , Gemini Observatory) There are 34 science targets in this mask. Tilted slits used for some galaxies in order to be able to measure rotation curves. Seeing during the observations was 0.7-1.0arcsec Abel 851 z = 0.4 Abel 851 z = 0.4

  12. GMOS: Evolution of ages and metalicity in Clusters from z= 1 to present epoch (Jørgensen 2002) The S/N needed for this type of work is 20-40 per Angstrom in the restframe of the cluster GMOS can deliver this. 5.5 hrs sky subtracted wavelength

  13. GMOS “Deep Deep Survey” 84 objects - 2 tiers with150 l/mm grating GDDS Team: Bob Abraham & Ray Carlberg (Toronto), Karl Glazebrook & Sandra Savaglio (JHU), Pat McCarthy (OCIW), David Crampton (DAO), Isobel Hook (Oxford), Inger Jørgensen & Kathy Roth (Gemini) Goal: Deep 100,000 sec MOS exposures on Las Campanas IR Survey fields to get redshifts of a complete K<20.5 sample to z=2 Access ‘redshift desert’ 1.2<z<2 FORMATION OF THE HUBBLE SEQUENCE This requires getting redshifts to I=24.5 - 1 mag fainter than Keck Lyman Break Galaxies. This requires good through-put, good image quality and “nod & shuffle” The GDDS team

  14. GMOS “Deep Deep Survey” 84 objects - 2 tiers with150 l/mm grating GDDS SV data: 14 hours in 0.5'' seeing (Aug 02) The GDDS team

  15. GDDS Nod & Shuffle 2 arcsec slit Shuffled imageof slit Shifted andsubtracted The GDDS team

  16. Example object: N&S subtracted I=23.8 z=1.07 [OII] 3727at 7700Å The GDDS team

  17. GDDS: ultra-super-preliminary results These are just the‘easy’ ones so far! Full 100,000 secswill pound on z=1.5old red galaxiesN&S works! Ultimate ‘sky null’ technique. Could reach I=27 in 106 secs on 30m The GDDS team

  18. Gemini South IR Performance and some results 4.7mm R=100,000 Rogers et al (in prep.)

  19. Flamingos / Gemini-S Flamingos on Gemini-S Deep J,H,K images in 1 field south of the Orion Core Total of 4hr integration - 0.4 arcsec images Preliminary ResultsJ,H,K Luminosity Functions show the expected peak near 0.3 M(solar)a slow decline or plateau in the brown dwarf regime (J~14.5 - 17.5 mag) for unreddened objectsA more rapid decline below the deuterium-burning limit and indications of a cut-off at a few M(Jupiter)Observations are complete to well below K=19mag. Lucas et al

  20. 3 - D data cube y 500 x 0.2” dispersed cells Integral Field Unit’s (IFU’s)enables “imaging spectroscopy” on Gemini  x 10 arcseconds HST galaxy, z = 0.6 (Lilly 1995)

  21. Interpretation courtesy Gerald Cecil Commissioning GMOS Integral Field Unit NGC 1068 GMOS IFU – [O III] 5007 1500 simultaneous spectra

  22. Wavelength/velocity [OII]3727 structure has two velocity components at +/-400km/s 3C324 3-D data cubeat z = 1.2 Y ( 5 arcsec ) X (7 arcsec) Bunker et al (2002)

  23. GEMINI-NORTH GMOS-IFU 10-15 June 2002 Cambridge IR Panoramic Survey Spectrograph GEMINI-SOUTH 4-9 August 2002

  24. CIRPASS early results– first use of anear-IR IFU on an 8m-class telescope. The example from the z=1.2 radio galaxy 3C324. Dispersion runs horizontally, spatial direction is vertical; each of the 500 IFU lenslets produces a spectrum 2 pixels high. The preliminary processing (basic sky subtraction and cosmic ray rejection) of this single 20 minute exposure shows a very clear detection of the redshifted [OIII] 500.7nm emission line (centre of the frame). http://www.gemini.edu/sciops/instruments/cirpass/cirpassDemoScience.html GMOS – IFU now available on Gemini North CIRPASS – IR IFU will be available on Gemini South in Service Mode in 2003A

  25. Challenges • Instruments, instruments, instruments…… • Gemini South will be without facility instruments until mid 2003 from the user perspective • And instrument delivery schedules constrain science availability of Gemini Telescopes

  26. Queue Observing Gemini’s queue support threshold Gemini-North Time Distribution Above 50% Classical time allocated New Instrument Mode Tests ALTAIR LGS NIFS Hokupa’a-S MICHELLE ALTAIR MICHELLE GMOS - N&S, GPOL NIRI - GPOL

  27. Queue Observing Gemini’s queue support threshold Gemini-South Time Distribution New Instrument Mode Tests NICI GNIRS NICI (cont.) GSAOI bHROS GMOS-S (cont.) FLAMINGOS-2 GSAO T-ReCS GMOS-S PHOENIX FLAMINGOS

  28. Future Challenges

  29. 2012 2015 Gemini N ? Gemini S 2000 2010 Exploring the Gemini context 2000 2010 SIRTF Keck I&II Keck-Inter. ESO-VLTI SOFIA NGST ALMA SIM VLA-upgrade SUBARU UT1,UT2,UT3,UT4 Magellan 1&2 HET LBT CELT LSST OWL VISTA and maybe GSMT… The decade of adaptive optics The era of the “giants”

  30. Exploring the Gemini context- and responding using Science Requirements 2000 2010 SIRTF Keck I&II Keck-Inter. ESO-VLTI SOFIA NGST ALMA SIM VLA-upgrade SUBARU UT1,UT2,UT3,UT4 Magellan 1&2 HET LBT CELT LSST OWL VISTA and maybe GSMT… Michelle NIFS 2012 2015 Gemini N ? ALTAIR + LGS GMOS Gemini S GAOS -> MCAO 2000 2010 GNIRS NICI Flam. 2 T-RECS The decade of adaptive optics The era of the “giants”

  31. R = 30,000 R = 5,000 R = 1,000 R = 5 Defining the role of Gemini in the era of a 6.5m NGST Assuming a detected S/N of 10 for NGST on a point source, with 4x1000s integration Time gain GEMINI advantage 1 102 NGST advantage 104

  32. Gemini’s Environment,“Aspen 2003”& our window of opportunity 2000 2010 SIRTF Keck I&II Keck-Inter. ESO-VLTI SOFIA NGST ALMA SIM VLA-upgrade SUBARU UT1,UT2,UT3,UT4 Magellan 1&2 HET LBT CELT LSST OWL VISTA and maybe GSMT… Mid-IR opportunity? Multi-IFU & MCAO++? Michelle NIFS 2012 2015 Gemini N ? ALTAIR + LGS GMOS Gemini S GAOS -> MCAO 2000 2010 Aspen 2003 GNIRS NICI Flam. 2 Extreme AO? T-RECS Seeing enhanced R=1,000,000 spectroscopy? The decade of adaptive optics The era of the “giants”

  33. Gemini’s Environment,“Aspen 2003”& our window of opportunity 2000 2010 SIRTF Keck I&II Keck-Inter. ESO-VLTI SOFIA NGST ALMA SIM VLA-upgrade In this evolving environment, timing as well as performance is key SUBARU UT1,UT2,UT3,UT4 Magellan 1&2 HET LBT CELT LSST OWL VISTA and maybe GSMT… Mid-IR opportunity? Multi-IFU & MCAO++? Michelle NIFS 2012 2015 Gemini N ? ALTAIR + LGS GMOS Gemini S GAOS -> MCAO 2000 2010 Aspen 2003 GNIRS NICI Flam. 2 Extreme AO? T-RECS Seeing enhanced R=1,000,000 spectroscopy? The decade of adaptive optics The era of the “giants”

  34. Our communities have struggled to deliver 8m – 10m class instruments 1.0 Slip Factor = original schedule + slip original schedule

  35. Thoughts so far…. • This current generation of 8m –10m telescopes can be extremely effective and efficient “science machines” • Queue Scheduling can make very effective use of these telescopes • Classical allocations are an essential ingredient for innovation – but requires significant time allocations • “Point and click astronomy” is here to stay • However, in this complex environment our continuing competitiveness requires targeted, state-of-the-art instrumentation, arriving at the telescope at the right time

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