Preparing AURA for the Next Generation AURA Board, Washington D.C 27 th February 2003

1. Preparing AURA for the Next Generation AURA Board, Washington D.C 27th February 2003

2. Preparing AURA for the Next Generation of Telescopes • Responding to the AASC Vision for Ground-based Astronomy • Involving the Astronomy Community in GSMT • Taking the Next StepPrepared by: Matt Mountain Jeremy Mould • Steve Strom Larry Stepp

3. Preparing AURA for the Next Generation of Telescopes Responding to the AASC Vision for Ground-based Astronomy • The scientific opportunities • The recommendations of the AASC • and European aspirations • Progress to date (in the US) • The CELT External Review • Two studies, one result • Science Case • Costs • First steps towards a GSMT

4. Preparing AURA for the Next Generation of Telescopes Involving the Astronomy Community in GSMT • Key AURA Accomplishments • GSMT Science Working Group • New Initiatives Office and the Point Design • Identifying technical challenges common to all ELT concepts • Site Evaluation • Integrated Modeling • Instrumentation Studies • AURA and the community will have to work together to develop new approaches for building $20M - $50M ELT Instruments

5. Preparing AURA for the Next Generation of Telescopes Taking the Next Step • The Competition is now Global • Non-US Capital investment is now 3x that of the US • The need for partnership • NIO Proposal to the NSF • Laying the foundation for a new Public – Private Partnership • Continuing to Involve the Community • Embracing a New Paradigm

6. The Scientific Opportunities21st Century astronomy is uniquely positioned to study “the evolution of the universe in order to relate causally the physical conditions during the Big Bang to the development of RNA and DNA” (R. Giacconi, 1997) Domain of the Next Generation Telescopes

7. Astronomy and Astrophysics in the New Millennium JWST ALMA GSMT LSST

8. AASC Vision for Ground-based Astronomy “The Giant Segmented Mirror Telescope (GSMT), the committee’s top ground-based recommendation….is a 30-m-class ground-based telescope that will be a powerful complement to NGST in tracing the evolution of galaxies and the formation of stars and planets.”

9. OWL 50m – 100m http://www.eso.org/projects/owl/index_2.html Astronomy and Astrophysics in Europe “we will not be left behind” JWST ALMA

10. AASC Vision for a Giant Segmented Mirror Telescope In addition to…OWL, there are three other programs in the early planning stages: MAXAT, a 30-50m telescope (NIO at NOAO), CELT 30-m class (Caltech & University of California), and ELT, a 25-m scale-up of the HET (Penn State & Texas). The GSMT described here corresponds closely with CELT or MAXAT. Although it is too early to judge the future direction of these projects, we believe that “GSMT could evolve directly from either of these initiatives, one from the private, the other from the public sector, or from a joint project created by the merging of these two.”

11. 30m Point Design Partnership between NOAO and Gemini Observatory Strengths Science The Gemini Observatory Wind and Structures Site Testing Adaptive Optics Instrumentation Two years ~ $2M Pre-Phase A and cost CELT Green Book Partnership between Caltech and University of California Strengths Science The Keck Observatory Optics Structures Adaptive Optics Instrumentation Two years ~ $2M Phase 1 and cost MAXAT 50m Progress to date (in the US) • CELT 30m Study • AURA NIO Study • External Review

12. Membership: Ed Moses – Project Director NIF Gary Sanders – Dep. Dir. LIGO Steve Shectman – PS Magellan Jerry Smith, Former Keck PM Ed Turner - Princeton Matt Mountain - Gemini Process Several pre-meetings of the Committee Detailed questions to CELT Team Two day review Final Report Observed by Wayne van Citters CELT External Review - September 2002 • Conclusions: • The Review Committee commends the design teamfor translating the visionary goal outlined in the Decadal Survey into a solid proof-of-principle concept • The Committee believes that the Universities could prudently engage in the next phase of the CELT project, the preliminarydesign, technology and vendor development phase.

13. Two Studies, One Result Results from 2 x 2 years of studies: • It is feasible to build a 30m Telescope that will fulfill the science objectives of theAASC, on a time scale comparable to JWST • The optics for a ~700m2 mirror can be manufactured, polished and assembled • Wind buffeting effects can be managed • The technologies exist or can be developed to enable diffraction limited imaging and spectroscopy in at least the IR • The instrumentation, though challenging, is within the capabilities of major institutions and industry • The cost for telescope construction, adaptive optics, initial instrumentation and including 30% contingency is between $600M - $700M

14. What the GSMT will do is: learn the physics of galaxy formation study the birth of stars and planets seek new biospheres The Science Case for a GSMT HST Witnessing assembly of galactic masses The physics of young Jupiter's Gemini x20 Log10 Fu (mJansky) GSMT with Ex-AO 2.0 4.0 l (mm) 8.0 Witness planets forming GSMT 30m telescope: resolution and light gathering power to analyze the physics of planets & galaxies

15. R = 10,000 R = 1,000 R = 5 Comparative performance of a 30m GSMT with a 25m2 JWST 30m GSMT point design Assuming a detected S/N of 10 for JWST on a point source, with 6x5000s integration GSMT advantage NGST advantage GSMT science strengths: Angular resolution and spectroscopy, the physics and dynamics of galaxies, stars and young planets

16. CELT & GSMT relative cost estimates • Independently derived – noticeable agreements and disagreements = lower = higher = agree

17. First Steps Toward a GSMT “The committee recommends that technology development for GSMT begin immediately and that construction start within the decade.” Astronomy and Astrophysics Survey Committee

18. JWST Launch Rapid Progress is Essential We already have 2 x 2 years of studies completed, A 2012 First Light requires a preliminary design by 2006

19. GSMT Full Construction Approval ALMA Construction GSMT D&D Phase Required GSMT Funding Profile Cumulative Total: $655M Partners NSF NIO A combination of public and private funds are required to deliver a GSMT in the 2012-2013 timeframe

20. Conceptual Design Challenges for Next Generation Telescopes Committed cost vs. program life cycle Early investment - reduces risk - maximizes science Starting in FY04 essential to completion early in JWST era Common challenges for all ELT concepts Community will have to work together to solve these problems and to develop key technologies Incurred cost GSMT 2012-2014 10% JWST 2010-2012 Conceptual design Optimize science and mitigate technical risks in Public-Private Partnership $70M initial investment - investigate high risks and “trade space” • Quantify wind buffeting effects • Active & Adaptive • controls design • Optics fabrication feasibility • Adaptive Optics • Cost-performance trades Private investment $35M NSF investment $35M FY’04 FY’05 FY’06

21. Critical Elements of a Community-Based Design Program • Quantify wind buffeting effects • Active & Adaptive controls design • Optics fabrication feasibility • Adaptive Optics • Cost-performance trades Site characterization Site prioritization Year 1 Year 2 Year 3 Preliminary Design integrated modeling Wind buffeting models and CFD studies System design Active and adaptive simulation studies Optical fabrication feasibility Optics evaluation End-to-end model infrastructure Cost-performance trades AO system models and simulation AO System design AO component development layered control systems active + adaptive systems wind flow system response

22. 03 04 05 06 07 08 09 10 ELT’s require broad national and international investment in key AO technologies End of Investment Start of Investment • 4 technologies: • high risk • High Power Lasers • Deformable • Mirrors • Low noise Detectors • System design Next generation CCD detectors Prototype Fiber Laser Next generation DM • 4 technologies: • low /moderate • risk • High Power Lasers • Deformable • Mirrors • Low noise Detectors • System Design Xinetics, 12” clear aperture MEMS~ 1 cm • Encourage commercial product lines • Estimated cost FY2004 through FY2010: $65M Investment now enables “next generation” and spins-off to current generation of telescopes 30m GSMT/CELT Full sky AO on current telescopes Optical AO on 4m’s Planet finders on 8-10m’s

23. Immediate Need: Funding for Design & Development Phase • $70M needed for DDP • Design & Simulation Tools • Site Evaluation • Technology Development • Preparing a Preliminary Design • NIO will seek $35M matching NSF funding • Focus on (1) – (3) broadly applicable to all ELT efforts • Proposal submission planned for June 2003 • Responsive to AASC recommendation that “technology development for GSMT begin immediately” • Provides community voice from inception of GSMT

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25. Key AURA Accomplishments to Date • Science Working Group for NSF convened • Initial science cases for GSMT developed • Initial performance requirements established • Core team of scientists and engineers in place • Point design developed • Key technical studies common to all ELT’s • Sites • Wind-buffeting • Integrated modeling • Instrument concepts • Cost, schedule and management model

26. GSMT Science Working Group The NSF GSMT SWG is a community-based group convened by NOAO to formulate a powerful science case for federal investment in GSMT • Identify key science drivers • Develop clear, compelling arguments for GSMT in era of JWST/ALMA • Discuss realization of science as a function of design parameters: • Aperture • FOV • Image quality • Etc. • Generate unified, coherent community support

27. GSMT SWG Members Chair: Rolf-Peter Kudritzki, UH IfA SWG Members: • Jill Bechtold -- UA • Mike Bolte -- UCSC • Ray Carlberg -- U of T • Matthew Colless -- ANU • Irena Cruz-Gonzales -- UNAM • Alan Dressler -- OCIW • Betsy Gillespie -- UA • Terry Herter -- Cornell • Jonathan Lunine -- UA LPL • Claire Max -- UCSC • Chris McKee -- UCB • Francois Rigaut -- Gemini • Chuck Steidel -- CIT • Doug Simons -- Gemini Vice Chair Steve Strom – NOAO

28. The physics of young Jupiter's Driving Science Themes GSMT • The Birth of Galaxies:The Archaeological Record • Characterize Exo-Planets • The Birth of Planetary Systems • The Birth of Galaxies: Witnessing the Process Directly • The Birth of Large-Scale Structure

29. The physics of young Jupiter's Science themes drive performance GSMT • For the majority of these themes, telescope aperture and image quality are key science drivers: • S/N a D2 – D3 • Sensitivity (1/time) a D4 – D6 Fully operational Adaptive Optics is a key Science Requirement for ELT’s

30. The physics of young Jupiter's Top Performance Requirements GSMT • Near-diffraction limited performance over ~ 2 arc-minute fields • High-dynamic-range imaging • High sensitivity mid-IR spectroscopy • Enhanced-seeing over ~ 5 arc-minute field • Wide-field, seeing-limited multi-object spectroscopy

31. GSMT SWG: Next Steps • Develop and vet key science cases • GSMT SWG + interaction with/contributions from the community • Provide input to NSF prior to June, 2003 • Justify substantial NSF investment in GSMT engineering studies

32. AURA New Initiatives Office Management Board William Smith -- President of AURA Jeremy Mould -- Director of NOAO Matt Mountain -- Director of Gemini Observatory Project Scientist Steve Strom Program Manager Larry Stepp System Scientist Brooke Gregory Admin. Assistant Holly Novack Clerk Jones - NOAO Opto-Mechanical Myung Cho Controls George Angeli Structures Paul Gillett Adaptive Optics TBD Software Development Anna Segurson Adaptive Optics Ellerbroek - Gemini Optics Robert Upton Structures Sheehan - Gemini Fluid Dynamics Konstantinos Vogiatzis Mechanical Designer Rick Robles Sites Walker - NOAO Instruments Barden - NOAO Optical Fabrication Hansen - Gemini Intern: Optomechanics Joon Pyo Lee Intern: Int. Modeling SoonJo Chung Intern: Adapt. Optics Ahmadia - Gemini

33. Results of Point Design Studies Design studies established feasibility • Design satisfies science requirements • Telescope design accommodates needed instruments • Technical challenges, but no show stoppers • AO components • Instrument components • Wind buffeting • Hierarchical control systems • Cost estimate consistent with decadal survey Identified technical challenges common to all ELT concepts

34. GSMT Site Evaluation • NIO collaborating with Carnegie, CELT, Cornell, ESO, UNAM; to test: • Las Campanas • Chajnantor • One or two additional Chilean Sites • Mauna Kea ELT site • San Pedro de Martir

35. Wind Site characterization has started Remote sensing CFD Simulations Weather stations Turbulence MASS • Status: • Erasmus remote sensing studies • MK / US / Chile comparison to finish in August • CFD modeling of sites: good progress on first three sites • Weather stations deployed on several mountains • Multi-Aperture Scintillation Sensor (MASS): • Performance verified by SCIDAR comparison • Manufacturing instruments for all sites

36. Comparison of Chilean Sites Site testing data available to all ELT Groups

37. Computational Fluid Dynamics • Characterize wind flow to allow pre-selection of sites • Wind intensity • Turbulence characteristics • Down-wind wakes • NIO has recruited CFD modeling expert -- Konstantinos Vogiatzis • Characterization of Chilean sites well underway • Analysis of other sites planned for 2nd Qtr 2003 Note: Gemini South site location chosen using only CFD analysis (CFD calibrated on MK, measurements later confirmed CP choice)

38. 500 m Wind Las Campanas Peak 2 Turbulent Kinetic Energy CFD Tools available for any proposed ELT site

39. Integrated Modeling • Goal: Simulate telescope and instrument performance in the presence of disturbances, corrected by active and adaptive systems • Value: • Accurately predict scientific performance • Guide critical engineering-science trades -- e.g., role of passive vs. active vs. adaptive systems • Essential tool for defining boundaries between groups, and coordinating and controlling costs • Enables scope of data taking and analysis software to be estimated • Combines several disciplines: • Dynamic Structural engineering -- finite-element analysis • Optical engineering -- ray tracing, Gaussian beam analysis • Adaptive optics -- AO simulation codes • Control system design -- models created in Matlab • Instrumentation – concepts and requirements determination An essential first step for this generation of ELT’s

40. Characterizing Effects of WindWind Measurements at Gemini South Ultrasonic anemometer • Wind data used as input for integrated modeling of telescope response under active control • CFD modeling will be used to scale to 30-m Pressure sensors Ultrasonic anemometer

41. Snapshot of Wind Pressure & Resulting Mirror Deformation Measured Wind Pressure (Pascals) Calculated Mirror Deformation on 30m • Unique data set made available on web • 116 five-minute test runs -- varying orientations and conditions • Resource used by multiple ELT projects

42. Dynamic Structural Modeling Preliminary 30m point design Successfully used to design and verify performance on Gemini Dynamic model requires 10,000+ nodes to determine the effects of wind on an Extremely Large Telescope structure

43. Adaptive Optics • Modeling new wave-front reconstruction techniques • Simulating AO performance of 30-m telescope • Using NIO “Beowulf” cluster • Evaluating effectiveness of laser guide star options • Evaluating challenging science cases • Proposal submitted to AFOSR • To port Ellerbroek’s comprehensive simulation code to the Maui supercomputer

44. 30” 20” 20” AO Simulation:Center of M32 Davidge et al. (2000) ~0.”12 FWHM H&K Gemini N + Hokupa’a Krist (1999) 8-m NGST PSF FWHM: 0.”032 J, 0.”057 K Sampling: 0.”035 pixels F. Rigaut GSMT PSF FWHM: 0.”009 J, 0.”015 K Sampling: 0.”005 pixels

45. AO Simulation Results GSMT NGST AO/MCAO modeling tools and simulations available to all ELT Groups (though you will need a super-computer)

46. Integrated Model of science performance is the result NIO developing techniques, tools and experience to assist multiple ELT programs

47. GSMT Instrument Studies AURA and the community will have to work together to develop new approaches for building $20M - $50M ELT Instruments

48. NIO Investments have already benefited the Community NIO efforts have focused on areas that benefit all ELT programs: • Solicited community input in defining key capabilities via science cases • Supported multiple site evaluation efforts • Provided extensive wind-buffeting database • Developed sophisticated adaptive optics simulation tools • Assembled engineering team with broadly applicable skills: • CFD modeling • Adaptive optics simulation • Integrated modeling of end-to-end system performance

49. We now have to take the next step…

50. OWL 100m The Competition is now Global Note: Non-US Capital investment is x 3 that of the US The time has arrived for a national US consensus on how to remain competitive on a global, not parochial scale