Preparing AURA for the Next Generation
AURA Board, Washington D.C
27th February 2003
1
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
2
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
3
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
4
Preparing AURA for the Next Generation
of Telescopes
Taking the Next Step
•
The Competition is now Global
–
•
•
The need for partnership
NIO Proposal to the NSF
–
•
•
Non-US Capital investment is now 3x that of the US
Laying the foundation for a new Public – Private Partnership
Continuing to Involve the Community
Embracing a New Paradigm
5
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)
6
Astronomy and Astrophysics in the
New Millennium
JWST
ALMA
LSST
GSMT
7
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.”
8
Astronomy and Astrophysics in Europe
“we will not be left behind”
JWST
ALMA
http://www.eso.org/projects/owl/index_2.html
9
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.”
10
Progress to date (in the US)
• AURA NIO Study
• 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
MAXAT
50m
– Pre-Phase
A and
cost
• CELT 30m Study
• 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
• External Review
11
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.
12
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 ~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
13
The Science Case for a GSMT
Witnessing assembly
of galactic masses
What the GSMT will do is:
learn the physics of galaxy formation
study the birth of stars and planets
seek new biospheres
HST
The physics of
young Jupiter's
Gemini
x20
GSMT with Ex-AO
2.0
4.0
l (mm)
8.0
Witness planets forming
GSMT
30m telescope: resolution and light gathering power to
14
analyze the physics of planets & galaxies
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
2
10.00
R = 10,000
R = 1,000
R= 5
1.00
NGST advantage
S/N Gain (GSMT / NGST)
R=5
R=1,000
R=10,000
GSMT
advantage
Comparative performance of a 25m JWST with a 30m GSMT
0.10
0.01
1
10
Wavelength (microns)
GSMT science strengths: Angular resolution and spectroscopy,
the physics and dynamics of galaxies, stars and young planets 15
CELT & GSMT relative cost estimates
• Independently derived – noticeable agreements and disagreements
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 Optics
Substantial difference – NIO leveraging Gemini MCAO
technology investment and expertise - operating MCAO
system in 2006
Contingency
GSMT carries 30%
Instrument will cost between
$20M - $50M each
Instruments
Total
$640M
= higher
CELT carries 22%
$610M
= lower
remarkable agreement of the
bottom-line
= agree
16
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
17
Rapid Progress is Essential
JWST Launch
We already have 2 x 2 years of studies completed,
A 2012 First Light requires a preliminary design by 2006
18
Required GSMT Funding Profile
$140
Cumulative Total: $655M
Yearly Spending (Million USD)
ALMA Construction
$120
$100
GSMT Full
Construction
Approval
$80
Partners
$60
$40
GSMT D&D Phase
NSF
$20
NIO
$0
2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013
A combination of public and private funds are required
to deliver a GSMT in the 2012-2013 timeframe
19
Conceptual Design Challenges for Next Generation
Telescopes
Committed cost vs. program life cycle
Early investment
- reduces risk
- maximizes
challenges
science
Common
for all ELT concepts
Incurred
cost
10%
Starting in FY04
essential to
Community will have
to work
completion early
together to solve these
problems
in JWST
era
GSMT 2012-2014
and to develop key technologies
Conceptual design
Optimize science and mitigate technical
risks in Public-Private Partnership
Private investment $35M
NSF investment $35M
FY’04
FY’05
FY’06
$70M initial
investment
- investigate
high risks
and
“trade space”
JWST 2010-2012
• Quantify wind
buffeting effects
• Active & Adaptive
controls design
• Optics fabrication
feasibility
• Adaptive Optics
• Cost-performance 20
trades
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
Wind buffeting models and CFD studies
Active and adaptive simulation studies
integrated
modeling
System design
Year 1 Year 2 Year 3
Optical fabrication feasibility
Optics evaluation
End-to-end model infrastructure
Cost-performance trades
AO system models and simulation
AO System design
AO component development
50
layered control systems
Zernike modes
aO (M1)
AO (M2)
temp.avg.
3
temp.avg.
Main Axes
Secondary
rigid body
temp.avg.
temp.avg.
Z
X
Y
system response
active + adaptive systems
20
2
wind flow
Preliminary
Design
0.01
0.1
1
10
Bandwidth [Hz]
100
21
ELT’s require broad national and international investment in
key AO technologies
End of Investment
Start of Investment
Prototype Fiber
Laser
4 technologies:
high risk
Next generation DM
Xinetics, 12” clear aperture
Next generation
CCD detectors
• High Power
Lasers
• Deformable
Mirrors
• Low noise
Detectors
• System design
MEMS~ 1
cm
• Encourage commercial product lines
• Estimated cost FY2004 through FY2010: $65M
03
Investment
now enables
“next
generation”
and spins-off
to current
generation of
telescopes
04
05
06
07
08
09
4 technologies:
low /moderate
risk
• High Power
Lasers
• Deformable
Mirrors
• Low noise
Detectors
•System Design
10
30m GSMT/CELT
Full sky AO on
current
telescopes
Optical AO on 4m’s
Planet finders on 8-10m’s
22
Immediate Need: Funding for
Design & Development Phase
• $70M needed for DDP
1.
2.
3.
4.
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
23
Involving
the Astronomy Community in
GSMT
an AURA responsibility
--- required by NSF
24 1
24
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
25
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
26
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
Vice Chair Steve Strom – NOAO
–
–
–
–
–
–
–
Terry Herter -- Cornell
Jonathan Lunine -- UA LPL
Claire Max -- UCSC
Chris McKee -- UCB
Francois Rigaut -- Gemini
Chuck Steidel -- CIT
Doug Simons -- Gemini
27
Driving Science Themes
GSMT
• The Birth of Galaxies:
The Archaeological Record
The physics of
young Jupiter's
• Characterize Exo-Planets
• The Birth of Planetary Systems
• The Birth of Galaxies:
Witnessing the Process Directly
• The Birth of Large-Scale Structure
28
Science themes drive performance
GSMT
The physics of
young Jupiter's
• 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
29
Top Performance Requirements
GSMT
• Near-diffraction limited performance
over ~ 2 arc-minute fields
The physics of
young Jupiter's
• High-dynamic-range imaging
• High sensitivity mid-IR spectroscopy
• Enhanced-seeing over ~ 5 arc-minute
field
• Wide-field, seeing-limited multiobject spectroscopy
30
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
31
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
Admin. Assistant
Holly Novack
System Scientist
Brooke Gregory
Clerk
Jones - NOAO
Opto-Mechanical
Myung Cho
Controls
George Angeli
Structures
Paul Gillett
Adaptive Optics
TBD
Optics
Robert Upton
Software Development
Anna Segurson
Structures
Sheehan - Gemini
Adaptive Optics
Ellerbroek - Gemini
Fluid Dynamics
Konstantinos Vogiatzis
Mechanical Designer
Rick Robles
Sites
Walker - NOAO
Instruments
Barden - NOAO
Intern: Optomechanics
Joon Pyo Lee
Intern: Int. Modeling
SoonJo Chung
Optical Fabrication
Hansen - Gemini
Intern: Adapt. Optics
Ahmadia - Gemini32
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
33
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
34
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
35
Comparison of Chilean Sites
1.0
T ransitional
Clear
Fraction
0.9
0.8
0.7
0.6
Y acas
Tronquitos
Toloncha
Tololo
Tolar
Q uimal
Q uanquero
Pena
Paranal
Infieles
G rande
Chascon
Chaco
Cascasco
0.5
Site testing data available to all ELT Groups
36
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)
37
Las Campanas Peak 2
Turbulent Kinetic Energy
500 m
CFD Tools available for any proposed ELT site
38
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
39
Characterizing Effects of Wind
Wind 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
Ultrasonic anemometer
Pressure sensors
40
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
41
Dynamic Structural Modeling
Preliminary
30m point
design
AVERAGE Pressure (C00030oo)
7
10
Z
6
10
5
10
Y
magnitude
X
4
10
3
10 Deformed(0.0673): Total Translation
Output Set: Mode 1, 2.156537 Hz,
Successfully used to design and
verify performance on Gemini
2
10
1
10
0
10
-3
10
SUM = -226
-2
-1
0
10
10
10
Frequency Response Function: frequency (Hz)
Dynamic model requires 10,000+ nodes to determine the
effects of wind on an Extremely Large Telescope structure
1
10
42
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
43
AO Simulation:
Center of M32
30”
20”
20”
Davidge et al. (2000)
Krist (1999) 8-m NGST PSF
F. Rigaut GSMT PSF
~0.”12 FWHM H&K
Gemini N + Hokupa’a
FWHM: 0.”032 J, 0.”057 K
Sampling: 0.”035 pixels
FWHM: 0.”009 J, 0.”015 K
Sampling: 0.”005 pixels
44
AO Simulation Results
GSMT
NGST
AO/MCAO modeling tools and simulations available
to all ELT Groups
(though you will need a super-computer)
45
Integrated Model of science performance is the result
NIO developing techniques, tools and experience to assist multiple
ELT programs
46
GSMT Instrument Studies
Instrument
Wavelength
Image
Resolution
Spectral
Resolution
FOV
Multiplex
MOMFOS
0.4 - 1 mm
1”
2000 - 20,000
20 arcmin
700
NIRDIF
1 - 2.5 mm
0.1” x 1”
5000 - 10,000
2 arcmin
26
MIHDAS
16 - 20 mm
0.2” (DL)
100,000
1 arcsec
1
1 - 5 mm
0.03” (DL)
100,000
0.1 arcsec
1
MCAO Imager
1 - 2.5 mm
0.03” (DL)
Imager
1.5 - 2
arcmin
1
MEIFU
0.4 - 1 mm
0.1” x
0.18”
500 - 1500
5 arcmin
5,000,000
1 - 5 mm
0.03” (DL)
Imager
2 arcsec
1
NIrES
Coronagraph
AURA and the community will have to work together to develop
new approaches for building $20M - $50M ELT Instruments
47
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
48
We now have to take the
next step…
49
The Competition is now Global
OWL 100m
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 50
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
51
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
52
NIO Proposal to NSF
Laying the foundation for a new
Public – Private Partnership
53531
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
Activities that benefit
all ELT programs
– Compare & evaluate proposed design concepts
– Produce a design for a 30m GSMT
54
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
55
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
56
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.”
57
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
58