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Gemini Observatory Report to the AURA Board 6 th February 2002

Gemini Observatory Report to the AURA Board 6 th February 2002. Highlights The AURA Review and the Gemini observing system Actions for AURA. …GG Tau Dan Potter, U of H. Gemini/Hokupa’a in K band Tidally truncated circumbinary disk Keplerian disk extent ~ 180-260 AU

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Gemini Observatory Report to the AURA Board 6 th February 2002

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  1. Gemini Observatory Report to the AURA Board 6th February 2002

  2. Highlights • The AURA Review and the • Gemini observing system • Actions for AURA

  3. …GG TauDan Potter, U of H • Gemini/Hokupa’a in K band • Tidally truncated circumbinary disk • Keplerian disk extent ~ 180-260 AU • Resolved imaging polarimetry of system • Nature of irregularities?

  4. Two ultracool companions to the young star HD130948Potter et al. 2001, ApJ submitted • Pair has same proper motion as primary • Gravitationally bound pair • Very low mass ultracool objects • Pair separation = 0.134+/-0.002” • Binary = 1.13 Msun total • Semi-major axis = 2.4 AU • period ~ 10 yr • Primary < 1 Gyr

  5. H=8 at 5 min

  6. …two ultracool companions: KECK/NIRSPEC spectroscopy • NIRSPEC fed by AO • KI, FeH, H2O bandheads • Both objects are dL2 • Contracting BDs • MB=0.075 Msun MC=0.065 Msun • First two BDs imaged around a G-type star

  7. Binary Brown Dwarf: 2M1426Close et al. (ApJL 2001 in press) • Hokupa’a on Gemini first ever to lock on a Brown Dwarf • 2M1426 is a very tight binary (3 AU) with a ~12 yr period

  8. … binary brown dwarf • 2M1426 system • M8.5 primary • L1 secondary • DUSTY models leads to a primary of 0.074 Msun and a secondary of 0.055 Msun • Fairly low mass companion for a BD

  9. Crossing the BD desert in 15 SgeLiu et al. 2002, ApJ, in press 0.06 Msun (48 Mjup) L dwarf companion HR 7672; 14 AU from star Gemini/Hokupa’a. BD can exist that close to the main star.

  10. Wolf-Rayet exports dust to the ISMTony Moffat et al. (U of Montreal) • Some Pop I WR stars are prolific dust producers • WC : T = 2.5 – 6 x 104 K • Dust shells to R ~ 103-4 R* • First imaging of WR dust envelopes in the mid IR • Extended dust envelope formed in wind-wind collision zone of P~25 yr WR+O binary. • Dust production is ~10-6 Msun yr-1. • 20% of “large grain” dust can escape from very hot stars into the ISM

  11. NIRI Status Supernova “Satie” • Science Verification data acquired in 2001 distributed to various teams • NIRI data processing IRAF package about to be distributed • Supernova Satie • Z=1.05 • J~24 mag • 2.5 hrs int. time (out of 8 hours total) • f/6 camera • 0.5 arcsec image quality • Awaiting acceptance… Gemini Observatory NIRI SV Team

  12. Gemini Multi-Object Spectrograph – 5.5’ x 5.5’ RXJO142+2131; z = 0.28 • FWHM • 0.50” • g’, r’, i’ • galaxies • in the 5.5’x5.5’ • field

  13. GMOS: object selection and examples of spectra

  14. Gemini South AURA Dedication of Gemini South a great success – thank you AURA!

  15. Gemini’s AD’s at work…. Gemini South Dedication A big “thank you” to Marylu Evans! - for herding, then re-herding the cats

  16. Gemini South ‘comes on line” NGC 6357 Star-forming Region in Scorpius NS14 Bipolar Nebula Recent (last night) Phoenix run was reporting 0.22 – 0.35” (K)

  17. Active nucleus observed at 4mm NGC 253 An edge-on starburst galaxy

  18. Gemini South + ABU + fast tip/tilt • Brackett  • FWHM ~ 0.35” • 1 minute integration The Galactic Center at Br-a- the power of IR optimization • Simons & Becklin 1992 • IRTF - L’ - Protocam • 16,000 images shift/add • An entire night….

  19. Recommendations of AURA’s Gemini Commissioning Review • R1 — Establish, measure, publicize and use clear metrics and milestones whereby commissioning progress can be quantified both for the benefit of the Gemini team and that of the broader Gemini community. • R2 — The schedule of telescope use on both Mauna Kea and Cerro Pachon must preserve, at all times, the flexibility to immediately attend to the repairs of unexpected system faults. This strategy must be maintained until the facility is "fully operational", i.e. the values of the metrics show all the performance goals to have been met. • R3 — Scheduling of instruments must primarily be guided at this time by their suitability and readiness to explore and test system's performance. Visitor instruments must be scheduled only when required for the commissioning of future, similar, facility instruments. • R4 — All science scheduling of the telescope must be in the queue mode or, for visitor instruments, in service observing mode. The intent here is to maintain the flexibility to revert to engineering work when required and to minimize the impact of visiting observers on the staff.

  20. National Time Allocation Process & ITAC Metrics - How do we quantify the scientific success or impact of an Observatory? The elements of this system under direct Gemini Control “Abingdon” workshops, new GSC (SWG’s), and Gemini Board Strategic planning and execution of instrumentation & development programs Gemini Board has funded IDF & FDF programs. Good project management applied across IDF & FDF + incentives (guaranteed time) Scientific outreach and Call for Proposals Over subscription rate Number of large projects Observatory gaining experience in both classical and queue scheduling, repeat rate in queue < 3% Queue scheduling Classical scheduling This is the Observatory’s operational challenge, improving performance, reliability and efficiency of the observing process Projects transformed to sequence of observations Instrument sensitivity Telescope reliability Observing efficiency Processing pipelines & quality assessment Conceptual design for Gemini Science Archive complete by CADC, Victoria Data archive or data mortuary Number of publications Number of citations Quantifiable Scientific Impact

  21. Metrics – target clear weather reliability(telescope + instruments) Gemini North (telescope only) requirement 100% 98% Telescope engineering/maintenance goal 80 Instrument commissioning 60 Clear weather reliability Gemini North 40 Gemini South Science availability 20 2002A 2002B 2003A 2003B 2004A

  22. Metrics – target observing efficiency [shutter open]/[elapsed time]Operationalfacility instruments 100% Telescope engineering/maintenance 85% goal 80 Instrument commissioning 60 requirement Observing efficiency 40 Science availability 20 2002A 2002B 2003A 2003B 2004A

  23. Total clear weather efficiency target and observing effectiveness • Define requirement as a fraction (percentage) of total clear weather time available, excluding the time used for instrument commissioning • 0.9 x 0.98 x 0.85 = 0.75 (if engineering, reliability and efficiency targets are met) • 75% of all available clear time should be used collecting ‘science photons’ • Define “observing effectiveness” of queue observing: The probability that the Observatory can complete highly ranked projects by matching observations to required atmospheric conditions • Queue simulations show that projects in ranking band 1, 95% of programs completed, band 2 (80%), and band 3 (50%) when scheduled as queued observations compared to 40% probability under classical scheduling (subject to random weather/atmospheric conditions) • Predicted observing effectiveness of Band 1 queued scheduled projects ~ 0.71 • Predicted observing effectiveness of classically scheduled projects ~ 0.75 x 0.4 = 0.3

  24. Benefits of Queue observing arise for three reasons: The Gemini instruments – like those of all new generation telescopes -- are complex machines and require training (and re-training). Gemini staff astronomers (and frequent visitors) can achieve and maintain a thorough level of understanding to operate the facility instruments at optimum efficiency. In the Classical mode, astronomers execute one program (or perhaps a backup program). In the Queue mode, each night is planned with between 6 to 9 programs; of these, parts of 2 up to 6 programs are executed in any given night. The key is that the queue allows for an optimal match between the science requirements of TAC approved programs, sky conditions and Right Ascensions.  In rapidly evolving conditions, the Gemini astronomers can interact with the PIs to explore a possible relaxation of the required conditions and are able to propose slight modifications in the way programs are executed. This again increases the probability of obtaining data matching the basic requirements of the PIs.

  25. Initial GMOS Queue Results • Observing efficiency in sequenced GMOS observations in imaging and MOS mode ~ 80%-85% • MOS acquisition < 10 mins. (required offsets ~ +/- 0.3”) • First GMOS Queue Run: “I have been observing on many ground-based telescopes for more than 32 years. I confess that from being a doubter of queue programming, I have swiftly become a full convert to the extraordinary advantages of queue observing. I am convinced that the Queue mode observing does double the amount of useful data coming from the new generations telescopes as compared to their use in a classical mode with visiting observers.” Dr. Jean-Rene Roy

  26. In this globally competitive environment AURA Board should conclude: • Gemini is beginning to produce world-class results • Both Keck and ESO are exploring “time swaps” with Gemini North • 2002-2003 will be critical years for the Observatory, we will be ramping up the Gemini science operations and the Gemini science production “machine”. • This success will in large part rely on a continued commitment by the largest partner, the US, both in terms of supporting this new way of doing facility based international astronomy, and through a continued partnership with the USGO and US instrument groups.

  27. In this globally competitive environment AURA Board should conclude: • Gemini does represent a “non-traditional” approach to groundbased observational O/IR astronomy. • However providing the broad US Community access to “an astronomy machine” and a fully supported groundbased archive (vis a vie ESO-VLT) is an essential element within the “diversity” of the US System • Gemini complements not competes with Keck, Magellan, HET, LBT etc.

  28. In this globally competitive environment AURA Board should conclude: 3. Continued competitiveness will rely on: • Groups (national/international consortia) focused on producing 8m class facility instruments • Traditional groundbased models are failing • Infrastructure requirements alone are beyond many University groups, many groups are only “one deep” Action: AURA should examine and encourage more cooperative models for building “world-class” 8m-10m scale instruments and find ways to develop the next generation of instrumentalists • The US community must become more fully enrolled in the opportunities, techniques and technologies for Adaptive Optics required to deliver forefront science in this new groundbased era. • Current funding models (PI grants) produces diverse but sub-critical results Action: AURA should support and promote a coherent AO Road Map within the US

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