1

Preparing AURA for the Next GenerationAURA Board, Washington D.C27th February 2003

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 MountainJeremy MouldSteve StromLarry Stepp

3

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

4

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

5

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

6

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)

7

Astronomy and Astrophysics in Astronomy and Astrophysics in the New Millenniumthe New Millennium

LSST GSMT

JWST ALMA

8

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.”

9

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

10

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.”

11

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

12

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.

13

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

14

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

15

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

16

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

17

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

18

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

19

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

20

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

21

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

22

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

23

• $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

24 1

Involving the Astronomy Community in

GSMTan AURA responsibility

--- required by NSF

24

25

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

26

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

27

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

28

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

29

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

30

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

31

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

32

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

33

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

34

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

35

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

36

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

37

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)

38

Las Campanas Peak 2 Las Campanas Peak 2 Turbulent Kinetic EnergyTurbulent Kinetic Energy

Wind

500 m

CFD Tools available for any proposed ELT site

39

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

40

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

41

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

42

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

43

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

44

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

45

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)

46

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

47

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

48

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

49

We now have to take the next step…

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 GlobalOWL 100m

51

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

52

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

53 1

NIO Proposal to NSF

Laying the foundation for a new Public – Private Partnership

53

54

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

55

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

56

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

57

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.”

58

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