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Lessons Learned Workshop 24 th August 2002

Lessons Learned Workshop 24 th August 2002. Success Challenges The Context for Aspen 2003 Looking ahead Timing as well as performance is key Data ………. Successes. IR Optimization works: Gemini-South IR (4 micron) Commissioning Images of Galactic Center. Simons & Becklin 1992

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Lessons Learned Workshop 24 th August 2002

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  1. Lessons Learned Workshop24th August 2002 • Success • Challenges • The Context for Aspen 2003 • Looking ahead • Timing as well as performance is key • Data ……….

  2. Successes

  3. 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

  4. 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

  5. Gemini South IR Performance

  6. GMOS North comes on-line GMOS on Gemini 5.5’ x 5.5’ 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 Telescope & instrument reliability > 90% Observing efficiency (shutter open/elapsed) Routinely ~ 70% PMN2314+0201 Quasar at z=4.11 Gemini SV PI: Isobel Hook

  7. GMOS “Deep Deep Survey” 84 objects - 2 tiers with150 l/mm grating The GDDS team

  8. GMOS “Deep Deep Survey” 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 -- using NOD & SHUFFLE Esp. virgin ‘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. GDDS SV data: 14 hours in 0.5'' seeing (Aug 02) The GDDS team

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

  10. 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

  11. 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”

  12. Exploring the Gemini context- and responding 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”

  13. Conclusions • The Gemini Partnership is capable of organizing itself to produce highly competitive, state-of-the-art facilities • “The Gemini whole” can be greater than the sum of the parts

  14. Challenges circa 2002 • Instrument delivery, instrument delivery, instrument delivery…… • Gemini South will be “bare” until mid 2003 from the user perspective • And instrument delivery schedules constrain science availability of Gemini Telescopes

  15. Gemini-North Time Distribution New Instrument Mode Tests ALTAIR LGS NIFS Hokupa’a-S MICHELLE ALTAIR MICHELLE GMOS - N&S, GPOL NIRI - GPOL

  16. 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

  17. Our communities have struggled to deliver instruments 1.0 Slip Factor = original schedule + slip original schedule Schedule Performance Data complied by Adrian Russell

  18. Looking Ahead

  19. 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

  20. 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”

  21. 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”

  22. Our record to date is not impressive 1.0 Slip Factor = original schedule + slip original schedule Schedule Performance Data complied by Adrian Russell

  23. And we have had to pay a significant price 1.0 Cost Overrun Factor = actual cost original approved budget Cost Impact (fully burdened) Data complied by Adrian Russell

  24. Thoughts so far…. • This current generation of 8m –10m telescopes can be extremely effective and efficient “science machines” • However, in this complex environment our continuing competitiveness requires targeted, state-of-the-art instrumentation, arriving at the telescope at the right time • And right now, we (at least Gemini) are not very good at this last bit…..

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