1. Gemini as Pathfinder for 21 st Century Astronmy Jean-René Roy Gran Telescopio Canarias Symposium – 25-26 July 2009

2. Who are we? Where are we ?

3. Sites 11,000 km apart + Gemini Science Archive in Canada Mauna Kea Cerro Pachon CADC-archive Total staff ~185 GN = 55% GS= 45% ~1/3 Eng ~1/3 Sci ~1/3 Admin + National Gemini Offices

4. 4 The universe from two hemispheres FUNDED BY United States United Kingdom Canada Australia Brazil Argentina Gemini North, Mauna Kea 4200 m Gemini South. Cerro Pachon 2900 m Twin Cassegrain 8 meter optical/infrared telescopes Optical, near infrared and mid infrared imagers and spectrographs Adaptive optics and integral field units

5. … Gemini : one observatory, two telescopes Since 2000 Gemini North, Hawaii Mauna Kea 4200 m

6. Gemini South, Chile Cerro Pachón 2900 m Since 2001

7. Gemini science niches for the ELTs era  Exoplanetary systems  Fine resolution spectral mapping  GRBs as first light “digging” sites Protoplanetary nebula NGC 7029 with GN Laser AO

8. Gemini ALTAIR/NIRI imaging of HR 8799 exoplanetary system 0.2” “

9. In 3rd quarter of 2008: a surprising crop of exoplanets! 8 M Jup in Beta Pic: VLT-NACO Gemini NKeck Gemini HR8799

10. Gemini Planet Imager GPI design: instrument being built by large consortiurm (LLNL, HIA, UC Santa Cruz, UCLA, AMNH). To be delivered at Gemini South in 2011.

11. NIRI+Altair Models of Young Planet Luminosity Marley et al. 2006 NICI 11 Age Planet Luminosity (L sun ) GPI

12. Integral field spectroscopy

13. Seth et al. 2008

14. … flashes from the beginning Artist view of gamma ray burst Gamma ray burst are still puzzling us for their progenitor event supernova explosion of “special” massive stars? or catastrophic merging of neutron stars/ black holes?

15. GRB 090423 at z ~ 8.3 Swift detected GRB 090423 on April 23 rd, 2009 at 3h55 am EDT –Follow up with Gemini GMOS-S & NIRI (also VLT, UKIRT, etc.) Photo-spectro z ~ 8.3 ! –Very massive star < 625 Myr after Big Bang GRB locations = proto- galaxy sites for ELTs Tanvir et al. 2009, Nature, in press

16. Joe Jensen 18 May 2009, Kyoto Queue observing and re-engaging astronomers with their machines

17. Queue/Classical at Gemini Gemini initial operational model was for 50% “queue”/service and 50% “classical” (PI at the telescope) User demand rapidly pushed to Q70-C30 around 2005 –Board/Agencies funded a “100% queue” in 2006- 2010 Staff astronomer at the telescope every night Currently queue is more than 90% of the Gemini N& S observing time

18. Henry Roe

19. Monitoring weather on Titan since 2003 NIRI/ALTAIR AO imaging monitoring of short-lived clouds (Schaller et al. 2009, Nature in press)

20. The “queue” Optimized execution of programs – Supernova Legacy Survey could not have been completed as a classical program High completion of highest ranked programs –Roll-over status High open shutter efficiency … but few astronomers at the telescope!

21. Ways to bring astronomers to the telescope As “classical” observers: we want more! –Several types of observations are still best done under with the PI at the telescope As Visiting Queue Observers (VQO) –Observer (especially PhD students and postdocs) with programs in the queue are invited to come to the observatory No guarantee but we will do every effort to execute some of their observations while they are present –VQOs will participate in many of the operational activities and to a few nights of queue observation Ideal duration of visit 2-4 weeks –Funding of expenses thru the NGOs or supervisor/team

22. “Time at the telescope was the most exciting of the visit. On a given night we would take up to six different types of observations: Coronagraphic imaging of exoplanets, Near Infrared (NIR) Integral Field Unit (IFU) observations of compact galaxies, multi-object spectroscopy. Being exposed to such a diversity of observations, I gained a deep appreciation for the difficulty of running such a wide array of instruments. However, the high point of my visit was being present when the last of my 2008B data, NIR observations of four gravitational lenses, were observed.” Ross Fadely (Rutgers University)* It is important to find clever ways to keep astronomers engaged with their machine and the observatory staff. * Visit at Gemini North in December 2008

23. Will ELTs be the last machines? ESO

24. … No! ESO 100 m Overwhelmingly Large telescope is in Phase B (Nov 2005 OWL Review) Concepts of single aperture ~50 m or array of km array (e.g. Mountain 1997) Currently planned GMT, TMT and E-ELT are not the final machines on the drawing board –Quantum efficiencies of detectors are close to one –Larger aperture (with image quality) is the only way for higher sensitivity from the ground

25. Lee Bennett 2004 Doc Ewen 2003 500 m FAST 100 m NRAO GBT NRL 600 ft Arecibo 305 m

27. Interferometry allows knowledge gain with unfilled aperture Sphere of molecular gas around T Lep (ESO/Le Bouquin) The surface of Altair ESO VLTI virtual aperture

28. Challenges Cost effectiveness of ground-based versus space Societal thresholds or barriers –Institutional and national science priorities –Funding constraints Necessity of large partnerships –Current market saturated: needs entry of Asian countries Benefits (and risks) of partnerships –E.g.UK in/out of Gemini? Key technologies –We may get less from NASA, DOE or DoD –We are more “on our own” with industry –Partnerships in mitigation strategies and projects Gemini and Keck joint lasers contract with LMCT

29. Reflections on partnership and lessons learned

30. Credit: Tetsuharu Fuse Subaru-Keck-Gemini: lasers and time exchange

31. 1993-2012 Gemini: a 20 yr international partnership  Gemini members are: United States (50%), United Kingdom (25%), Canada (15%), Australia (5%) Argentina (2.5%) and Brazil (2.5%) - Hosts: Chile, Hawaii  Current Gemini International Agreement ends on 31 Dec. 2012. Negotiations for renewed partnership post-2012 have started.  Renewable partnership has advantages but is source of uncertainty  E.g. UK membership ?

32. Asymmetric partnerships Gemini partnership and shares –USA* (50.1%) –United Kingdom* (23.8%) –Canada* (15%) –Australia (6.2%) –Brazil (2.5%) –Argentina (2.4%) Asymmetry is not an issue –But having partners with too small a share is questionable Perception of “voice not heard” Impediment to participation in the instrumentation program Community could use effectively and productively a larger share of telescope time –And when a large partner runs into financial difficulty…. * Have veto power on“financial” matters

33. “Distributed” model for user support: the NGO system Each Gemini partner funds/supports/operates a National Gemini Office, including hosts –Handles and controls initial proposal and TAC process –Provides “first-line” support (e.g. Tier one of HelpDesk) Phase I and Phase II of proposal support –Acts as interface between user community and observatory Following a “rough start”, Gemini “distributed” system is now much better –Can provide more timely response in a multi-time zone Strength, depth and quality of NGO support depend on staff –Staff rotates; small NGOs are challenged by the multiple instruments and wide capabilities

34. Multi TAC Gemini does not handle nor control the Time Allocation Process, except in its ultimate steps NINE TACS (six partners/two hosts/one GemStaff TACs) assess, select and recommend each a ranked list of proposals (each must match weather requirements probability) The International TAC receives/merges and recommends a final list to the Gemini director Multi-TAC is very fragmented –Impediment to large programs with significant allocation of time; “joint” programs impacted by multiple jeopardy –Long-term status is almost impossible unless strongly endorsed by a large partner

35. 2010-2020: the 8-10 m decade 2010-2020 = a promising decade with JWST and ALMA coming on line before mid-decade –As HST did, these facilities will have huge impact scientifically and influence the way ground-based telescopes operate PANSTARS, VISTA, LSSTs (and others) will demand rapid/efficient “point-and-shoot” spectroscopic follow up –Current 8-10 m have to become even more “responsive” Operational ELTs with instrumentation will come on line late in the coming decade or first half of 2020 Current generation of 8-10 m has q 10-year window of a scientific “freeway” ahead with a generous discover space

36. Governance

37. ¡ Muchas gracias y buena suerte al GTC !