1 preparing aura for the next generation aura board, washington d.c 27 th february 2003
TRANSCRIPT
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Preparing AURA for the Next GenerationAURA Board, Washington D.C27th February 2003
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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 MountainJeremy MouldSteve StromLarry Stepp
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Preparing AURA for the Next Preparing AURA for the Next Generation of TelescopesGeneration 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
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Preparing AURA for the Next Preparing AURA for the Next Generation of TelescopesGeneration 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
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Preparing AURA for the Next Preparing AURA for the Next Generation of TelescopesGeneration 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
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The Scientific OpportunitiesThe Scientific Opportunities
21st Century astronomy is uniquely positioned to study “21st Century astronomy is uniquely positioned to study “the the evolution of the universe in order to relate causally the physical evolution of the universe in order to relate causally the physical
conditions during the Big Bang to the development of RNA and DNA” conditions during the Big Bang to the development of RNA and DNA” (R. Giacconi, 1997)(R. Giacconi, 1997)
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Astronomy and Astrophysics in Astronomy and Astrophysics in the New Millenniumthe New Millennium
LSST GSMT
JWST ALMA
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AASC Vision for Ground-based AASC Vision for Ground-based AstronomyAstronomy
“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.”
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Astronomy and Astrophysics in Astronomy and Astrophysics in Europe “Europe “we will not be left behindwe will not be left behind””
http://www.eso.org/projects/owl/index_2.html
OW
L
50m
– 1
00m
JWST ALMA
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AASC Vision for a Giant AASC Vision for a Giant Segmented Mirror TelescopeSegmented 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.”
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MAXAT 50m
Progress to date (in the Progress to date (in the US)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
• CCELT Green BookELT 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
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CELT External Review - CELT External Review - September 2002September 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 preliminarydesign, technology and vendor development phase.
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Two Studies, One ResultTwo Studies, One ResultResults 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 ~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
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The Science Case for a GSMTThe Science Case for a GSMT
What the GSMT will do is:What the GSMT will do is: learn the physics of galaxy formationlearn the physics of galaxy formation study the birth of stars and planetsstudy the birth of stars and planets seek new biospheresseek new biospheres
Witnessing assembly of galactic masses
Witness planets forming
30m telescope: resolution and light gathering 30m telescope: resolution and light gathering power to analyze the physics of planets & galaxiespower to analyze the physics of planets & galaxies
HST
GSMT
Lo
g1
0 F
(
Jan
sky)
2.0 4.0 m) 8.0
x20
Gemini
GSMT with Ex-AO
The physics of young Jupiter's
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Comparative performance of a 30m GSMT with a Comparative performance of a 30m GSMT with a 25m25m22 JWST 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
1 100.01
0.10
1.00
10.00
Comparative performance of a 25m2JWST with a 30m GSMT
S/N
Gai
n (G
SMT
/ NG
ST)
Wavelength (microns)
R=5 R=1,000 R=10,000 R = 10,000 R = 1,000 R = 5
GS
MT
a
dv
an
tag
eN
GS
T a
dv
an
tag
e
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CELT & GSMT relative cost estimatesCELT & GSMT relative cost estimates
GSMT CELT Comments
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 OpticsSubstantial difference – NIO leveraging Gemini MCAO technology investment and expertise - operating MCAO system in 2006
Contingency GSMT carries 30% CELT carries 22%
InstrumentsInstrument will cost between
$20M - $50M each
Total $640M $610M remarkable agreement of the bottom-line
• Independently derived – noticeable agreements and disagreements
= higher = lower = agree
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First Steps Toward a GSMTFirst 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
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Rapid Progress is Rapid Progress is EssentEssentialial
JWST Launch
We already have 2 x 2 years of studies completed, A 2012 First Light requires a preliminary design by 2006
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Required GSMT Funding Required GSMT Funding ProfileProfile
$0
$20
$40
$60
$80
$100
$120
$140
2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013
Yea
rly
Sp
end
ing
(M
illio
n U
SD
) 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
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Conceptual Design Challenges for Next Conceptual Design Challenges for Next Generation TelescopesGeneration Telescopes
10%10%
IncurredcostIncurredcost
Committed cost vs. program life cycle Committed cost vs. program life cycle
FY’04 FY’05 FY’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 2012-2014GSMT 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 technicalrisks 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
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Critical Elements of a Community-Based Critical Elements of a Community-Based Design ProgramDesign Program
• Quantify wind buffeting effects
• Active & Adaptive controls design
• Optics fabrication feasibility
• Adaptive Optics
• Cost-performance trades
X Y
Z
Output Set: Mode 1, 2.156537 Hz, Deformed(0.0673): Total Translation
2
3
20
50
0.1 10 1001
Bandwidth [Hz]
Zern
ike m
odes
0.01
AO (M2)
Secondaryrigid body
Main Axes
temp.avg.
temp.avg.
temp.avg.
temp.avg.
aO (M1)
Year 1 Year 2 Year 3Site characterization
Wind buffeting models and CFD studies
Active and adaptive simulation studies
Optical fabrication feasibility
Site prioritization
End-to-end model infrastructure
integratedmodeling
Cost-performance tradesOptics evaluation
System designPreliminary
Design
wind flow system response
layered control systemsactive + adaptive systems
AO system models and simulationAO component development AO System design
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ELT’s require broad national and international ELT’s require broad national and international investment in key AO technologiesinvestment 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’s Planet finders on 8-10m’s
Full sky AO on current
telescopes
30m GSMT/CELTInvestmentnow enables “nextgeneration” and spins-off to currentgeneration of telescopes
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• $70M needed for DDP1. Design & Simulation Tools2. Site Evaluation3. Technology Development4. 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 Immediate Need: Funding for Design & Development PhaseDesign & Development Phase
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Involving the Astronomy Community in
GSMTan AURA responsibility
--- required by NSF
24
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Key AURA Accomplishments Key AURA Accomplishments to Dateto 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
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GSMT Science Working GSMT Science Working GroupGroup
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
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GSMT SWG MembersGSMT 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
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Driving Science ThemesDriving 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
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Science themes drive Science themes drive performanceperformance
• For the majority of these themes, telescope aperture and image quality are key science drivers:
• S/N D2 – D3 • Sensitivity
(1/time)D4 – D6
The physics of young Jupiter's
GSMT
Fully operationalAdaptive Optics is a key Science Requirement for ELT’s
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Top Performance Top Performance RequirementsRequirements
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
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GSMT SWG: Next StepsGSMT 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
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AURA New Initiatives OfficeAURA New Initiatives Office
Management BoardWilliam Smith -- President of AURA
Jeremy Mould -- Director of NOAO
Matt Mountain -- Director of Gemini Observatory
Project ScientistSteve Strom
Program ManagerLarry Stepp
System ScientistBrooke Gregory
Mechanical DesignerRick Robles
Admin. AssistantHolly Novack
Opto-MechanicalMyung Cho
Structures
Paul Gillett
ControlsGeorge Angeli
Adaptive OpticsEllerbroek - Gemini
InstrumentsBarden - NOAO
Adaptive Optics
TBD
Sites
Walker - NOAO
Fluid DynamicsKonstantinos Vogiatzis
Optics
Robert Upton
Software DevelopmentAnna Segurson
Intern: Int. ModelingSoonJo Chung
Intern: OptomechanicsJoon Pyo Lee
ClerkJones - NOAO
StructuresSheehan - Gemini
Intern: Adapt. OpticsAhmadia - Gemini
Optical Fabrication
Hansen - Gemini
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Results of Point Design Results of Point Design StudiesStudies
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
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GSMT Site EvaluationGSMT 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
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Site characterization has Site characterization has startedstarted
Remote sensing
Wind
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
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Comparison of Chilean Comparison of Chilean SitesSites
0.5
0.6
0.7
0.8
0.9
1.0C
asca
sco
Cha
co
Cha
scon
Gra
nde
Infie
les
Par
anal
Pen
a
Qua
nque
ro
Qui
mal
Tol
ar
Tol
olo
Tol
onch
a
Tro
nqui
tos
Yac
as
Fra
ctio
n
Transitional
Clear
Site testing data available to all ELT Groups
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Computational Fluid Computational Fluid DynamicsDynamics
• 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)
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Las Campanas Peak 2 Las Campanas Peak 2 Turbulent Kinetic EnergyTurbulent Kinetic Energy
Wind
500 m
CFD Tools available for any proposed ELT site
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Integrated ModelingIntegrated 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
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Characterizing Effects of WindCharacterizing Effects of Wind Wind Measurements at Gemini South
Pressure sensors
Ultrasonic anemometer
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
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Snapshot of Wind Pressure Snapshot of Wind Pressure & Resulting Mirror Deformation& 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
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Dynamic Structural Dynamic Structural ModelingModeling
Successfully used to design andverify performance on Gemini
X Y
Z
Output Set: Mode 1, 2.156537 Hz, Deformed(0.0673): Total Translation
10-3
10-2
10-1
100
101
100
101
102
103
104
105
106
107
Frequency Response Function: frequency (Hz)
mag
nitu
de
AVERAGE Pressure (C00030oo)
SUM = -226
Preliminary30m pointdesign
Dynamic model requires 10,000+ nodes to determine the effects of wind on an Extremely Large Telescope structure
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Adaptive OpticsAdaptive 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
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AO Simulation:AO Simulation:Center of M32Center of M32
Davidge et al. (2000)
~0.”12 FWHM H&KGemini N + Hokupa’a
Krist (1999) 8-m NGST PSF
FWHM: 0.”032 J, 0.”057 K Sampling: 0.”035 pixels
30” 20” 20”
F. Rigaut GSMT PSF
FWHM: 0.”009 J, 0.”015 K Sampling: 0.”005 pixels
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AO Simulation ResultsAO Simulation Results
NGST
GSMT
AO/MCAO modeling tools and simulations available to all ELT Groups
(though you will need a super-computer)
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NIO developing techniques, tools and experience to assist multiple ELT programs
Integrated Model of Integrated Model of science performancescience performance is is the result the result
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GSMT Instrument StudiesGSMT Instrument Studies
Instrument Wavelength
Image Resolution
Spectral Resolution
FOV Multiplex
MOMFOS 0.4 - 1 m 1” 2000 - 20,000
20 arcmin
700
NIRDIF 1 - 2.5 m 0.1” x 1” 5000 - 10,000
2 arcmin 26
MIHDAS 16 - 20 m 0.2” (DL) 100,000 1 arcsec 1
NIrES 1 - 5 m 0.03” (DL) 100,000 0.1 arcsec
1
MCAO Imager
1 - 2.5 m 0.03” (DL) Imager 1.5 - 2 arcmin
1
MEIFU 0.4 - 1 m 0.1” x 0.18”
500 - 1500 5 arcmin 5,000,000
Coronagraph
1 - 5 m 0.03” (DL) Imager 2 arcsec 1
AURA and the community will have to work together to developnew approaches for building $20M - $50M ELT Instruments
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NIO Investments have NIO Investments have alreadyalready benefited the benefited the
CommunityCommunityNIO 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
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We now have to take the next step…
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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 GlobalOWL 100m
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The Need for PartnershipThe 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
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Partnership OpportunityPartnership 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
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NIO Proposal to NSF
Laying the foundation for a new Public – Private Partnership
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Preparing for the New Preparing for the New “Public- Private” Paradigm“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
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Activities That Benefit Activities That Benefit All ELT ProgramsAll 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
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Plan to continue involving Plan to continue involving the communitythe 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
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Embracing a New ParadigmEmbracing 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.”
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Embracing a New ParadigmEmbracing 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