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

2. 2 Preparing AURA for the Next Generation of Telescopes 1.Responding to the AASC Vision for Ground-based Astronomy 2.Involving the Astronomy Community in GSMT 3.Taking the Next Step Prepared by: Matt Mountain Jeremy Mould Steve Strom Larry Stepp

3. 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. 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. 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. 6 The Scientific Opportunities 21st 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)

7. 7 Astronomy and Astrophysics in the New Millennium LSST GSMT JWSTALMA

8. 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. 9 Astronomy and Astrophysics in Europe “we will not be left behind” http://www.eso.org/projects/owl/index_2.html OWL 50m – 100m JWSTALMA

10. 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. 11 MAXAT 50m Progress to date (in the US) AURA NIO Study CELT 30m Study External Review 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 C ELT Green Book C ELT 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

12. 12 CELT External Review - September 2002 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 Conclusions: 1.The Review Committee commends the design team for translating the visionary goal outlined in the Decadal Survey into a solid proof-of-principle concept 2.The Committee believes that the Universities could prudently engage in the next phase of the CELT project, the preliminary design, technology and vendor development phase.

13. 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 the AASC, on a time scale comparable to JWST –The optics for a ~700m 2 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. 14 The Science Case for a GSMT The Science Case for a GSMT What the GSMT will do is: learn the physics of galaxy formation learn the physics of galaxy formation study the birth of stars and planets study the birth of stars and planets seek new biospheres seek new biospheres Witnessing assembly of galactic masses Witness planets forming 30m telescope: resolution and light gathering power to analyze the physics of planets & galaxies HST GSMT Log 10 F  (  Jansky) 2.04.0  m) 8.0 x20 Gemini GSMT with Ex-AO The physics of young Jupiter's

15. 15 Comparative performance of a 30m GSMT with a 25m 2 JWST 30m GSMT point design Assuming a detected S/N of 10 for JWST on a point source, with 6x5000s integration GSMT science strengths: Angular resolution and spectroscopy, the physics and dynamics of galaxies, stars and young planets R = 10,000 R = 1,000 R = 5 GSMT advantage NGST advantage

16. 16 CELT & GSMT relative cost estimates GSMTCELTComments Optics NIO estimates for M1 & adaptive M2 ~ $110M Telescope Agreement within 15% Enclosure $10M difference may be design approach Base Facility CELT = 4 x GSMT Control System CELT Review believed this underestimated Adaptive Optics Substantial difference – NIO leveraging Gemini MCAO technology investment and expertise - operating MCAO system in 2006 Contingency GSMT carries 30% CELT carries 22% Instruments Instrument will cost between $20M - $50M each Total$640M$610M remarkable agreement of the bottom-line Independently derived – noticeable agreements and disagreements = higher = lower = agree

17. 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. 18 Rapid Progress is Essent ial JWST Launch We already have 2 x 2 years of studies completed, A 2012 First Light requires a preliminary design by 2006

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

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

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

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

23. 23 $70M needed for DDP 1.Design & Simulation Tools 2.Site Evaluation 3.Technology Development 4.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 Immediate Need: Funding for Design & Development Phase

24. 24

25. 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. 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. 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. 28 Driving Science Themes The physics of young Jupiter's 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 GSMT

29. 29 Science themes drive performance For the majority of these themes, telescope aperture and image quality are key science drivers: S/N  D 2 – D 3 Sensitivity (1/time)  D 4 – D 6 The physics of young Jupiter's GSMT Fully operational Adaptive Optics is a key Science Requirement for ELT’s

30. 30 Top Performance Requirements The physics of young Jupiter's 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 GSMT

31. 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. 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 Mechanical Designer Rick Robles Admin. Assistant Holly Novack Opto-Mechanical Myung Cho Structures Paul Gillett Controls George Angeli Adaptive Optics Ellerbroek - Gemini Instruments Barden - NOAO Adaptive Optics TBD Sites Walker - NOAO Fluid Dynamics Konstantinos Vogiatzis Optics Robert Upton Software Development Anna Segurson Intern: Int. Modeling SoonJo Chung Intern: Optomechanics Joon Pyo Lee Clerk Jones - NOAO Structures Sheehan - Gemini Intern: Adapt. Optics Ahmadia - Gemini Optical Fabrication Hansen - Gemini

33. 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. 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. 35 Site characterization has started Remote sensing Wind CFD SimulationsWeather stationsTurbulence 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. 36 Comparison of Chilean Sites Site testing data available to all ELT Groups

37. 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. 38 Las Campanas Peak 2 Turbulent Kinetic Energy Wind 500 m CFD Tools available for any proposed ELT site

39. 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. 40 Characterizing Effects of Wind Characterizing Effects of Wind Wind Measurements at Gemini South Pressure sensors 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

41. 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. 42 Dynamic Structural Modeling Successfully used to design and verify performance on Gemini Preliminary 30m point design Dynamic model requires 10,000+ nodes to determine the effects of wind on an Extremely Large Telescope structure

43. 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. 44 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 30”20” F. Rigaut GSMT PSF FWHM: 0.”009 J, 0.”015 K Sampling: 0.”005 pixels

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

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

47. 47 GSMT Instrument Studies InstrumentWavelengthImage Resolution Spectral Resolution FOVMultiplex MOMFOS0.4 - 1  m1”2000 - 20,00020 arcmin700 NIRDIF1 - 2.5  m0.1” x 1”5000 - 10,0002 arcmin26 MIHDAS16 - 20  m0.2” (DL)100,0001 arcsec1 NIrES1 - 5  m0.03” (DL)100,0000.1 arcsec1 MCAO Imager1 - 2.5  m0.03” (DL)Imager1.5 - 2 arcmin 1 MEIFU0.4 - 1  m0.1” x 0.18” 500 - 15005 arcmin5,000,000 Coronagraph1 - 5  m0.03” (DL)Imager2 arcsec1 AURA and the community will have to work together to develop new approaches for building $20M - $50M ELT Instruments

48. 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. 49 We now have to take the next step…

50. 50 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 The Competition is now Global OWL 100m

51. 51 The Need for Partnership Advancing a GSMT depends on partners who: –Can provide funds to complement anticipated NSF investment –Are committed to a public/private partnership to build a 30-m telescope as envisioned by AASC: Contemporary with JWST Involving community during all project phases

52. 52 Partnership Opportunity UC and Caltech are prepared to partner with AURA to design a 30m CELT/GSMT Canadian Universities (ACURA) are interested in partnering in a 30m CELT/GSMT –Caltech and UC funding via proposal to Moore Foundation –Proposed Canadian funding via ACURA proposal to CFI –Proposed NIO contributions: NIO engineering team Funds from a successful proposal to NSF ($35M) Partners ready to initiate joint D&D Phase –Building on point design studies

53. 53 Laying the foundation for a new Public – Private Partnership 53

54. 54 Preparing for the New “Public- Private” Paradigm NIO will request $35M in NSF funds to provide a public match to: –UC and Caltech funding request to Moore Foundation –ACURA funding request to CFI NIO portion will assure public participation during the design phase of the project recommended by the AASC Together these funds will: –Develop key technologies and components –Address fundamental ELT design issues –Evaluate candidate sites –Compare & evaluate proposed design concepts –Produce a design for a 30m GSMT Activities that benefit all ELT programs

55. 55 Activities That Benefit All ELT Programs Engage our communities in AASC vision for GSMT Champion community science interests Analyze and model telescope wind buffeting effects Develop AO simulation codes & predict system performance Develop integrated modeling tools & end-to-end simulations Evaluate key science-engineering trade studies Evaluate premier site candidates Fund development of advanced adaptive optics components Fund development of instrument design concepts Fund key instrument technology developments Fund development of high-performance coatings Establish accepted software architecture & standards Explore operations options and cost models

56. 56 Plan to continue involving the community Maintain the GSMT SWG beyond its NSF report Ongoing science scrutiny of performance trades –community science workshops –science drivers for instrumentation –data management and NVO interface Form (continue) an Institutional Support Consortium Opportunity to draw on institutional skills –Science simulations; technical innovations, instrument development Consolidating resource pool Forum for adaptive optics exchange

57. 57 Embracing a New Paradigm The proposed partnership matches the AASC vision: “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.”

58. 58 Embracing a New Paradigm The proposed partnership matches the AASC vision AURA stands ready to advance the AASC vision –Partner with Caltech, UC and Canada –Support ELT technology development AURA is ready to ensure: –our community has access to a state-of-the-art GSMT –US leadership in this Millennium