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Gemini as Pathfinder for 21 st Century Astronmy Jean-René Roy. Gran Telescopio Canarias Symposium – 25-26 July 2009. Who are we? Where are we ?. Sites 11,000 km apart + Gemini Science Archive in Canada. Total staff ~185 GN = 55% GS= 45% ~1/3 Eng ~1/3 Sci ~1/3 Admin + National - PowerPoint PPT Presentation
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Gemini as Pathfinder for21st Century Astronmy
Jean-René Roy
Gran Telescopio Canarias Symposium – 25-26 July 2009
Who are we?Who are we?Where are we ?Where are we ?
Sites 11,000 km apart + Gemini Science Archive in Canada
Mauna Kea
Cerro Pachon
CADC-archiveCADC-archive
Total staff~185
GN = 55%GS= 45%
~1/3 Eng~1/3 Sci~1/3 Admin+ NationalGeminiOffices
4
The universe from two hemispheres
FUNDED BYFUNDED BY United States United Kingdom Canada AustraliaBrazil 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
… Gemini : one observatory, two telescopes
Since 2000
Gemini North, HawaiiMauna Kea 4200 m
Gemini South, ChileCerro Pachón 2900 m Since 2001
Gemini science niches for the ELTs era
Exoplanetary systemsFine resolution spectral mappingGRBs as first light “digging” sites
Protoplanetary nebula NGC 7029 with GN Laser AO
Gemini ALTAIR/NIRI imaging of HR 8799 exoplanetary system
0.2” “
In 3rd quarter of 2008: a surprising crop of exoplanets!
8 MJup in Beta Pic: VLT-NACO
Gemini N Keck
GeminiHR8799
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.
NIRI+Altair
Models of Young Planet Luminosity
Marley et al. 2006
NICI
11Age
Pla
net L
umin
osit
y (L
sun)
GPI
Integral field spectroscopy
Seth et al. 2008
… flashes from the beginning
Artist view of gamma ray burst
Gamma ray burstare still puzzling us for their progenitor event
supernova explosionof “special” massive stars? or catastrophic merging ofneutron stars/ black holes?
GRB 090423 at z ~ 8.3
• Swift detected GRB 090423 on April 23rd, 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
Joe Jensen
18 May 2009, Kyoto
Queue observing and re-engaging astronomers
with their machines
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
Henry Roe
Monitoring weather on Titansince 2003
NIRI/ALTAIR AO imaging monitoring of short-lived clouds(Schaller et al. 2009, Nature in press)
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!
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
• “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 engagedwith their machine and the observatory staff.
* Visit at Gemini North in December 2008
Will ELTs be the last machines?
ESO
… 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
Lee Bennett 2004
Doc Ewen 2003
500 m FAST
100 m NRAO GBT
NRL 600 ft
Arecibo 305 m
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
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
Reflections on partnership and lessons learned
Credit: Tetsuharu Fuse
Subaru-Keck-Gemini: lasers and time exchange
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 uncertaintyE.g. UK membership ?
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
“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
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
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
Governance
¡ Muchas gracias y buena suerte al GTC !
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