Preparing AURA for the Next Generation

1
Preparing AURA for the Next Generation AURA
Board, Washington D.C 27th February 2003
2

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

3
Preparing AURA for the Next Generation of
Telescopes

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

4
Preparing AURA for the Next Generation of
Telescopes

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

5
Preparing AURA for the Next Generation of
Telescopes

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

6
The Scientific Opportunities21st Century
astronomy is uniquely positioned to study the
evolution of the universe in order to relate
causally the physical conditions during the Big
Bang to the development of RNA and DNA (R.
Giacconi, 1997)
Domain of the Next Generation Telescopes
7
Astronomy and Astrophysics in the New Millennium
JWST
ALMA
GSMT
LSST
8
AASC Vision for Ground-based Astronomy
The Giant Segmented Mirror Telescope (GSMT), the
committees 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 Europe we will not
be left behind
JWST
ALMA
10
AASC Vision for a Giant Segmented Mirror Telescope
In addition toOWL, 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
Progress to date (in the US)

• CELT 30m Study

• 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
• Pre-Phase A and cost

• CELT Green Book
• Partnership between Caltech and University of
  California
• Strengths
• Science
• The Keck Observatory
• Optics
• Structures
• Adaptive Optics
• Instrumentation
• Two years 2M
• Phase 1 and cost

• External Review

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
• The Review Committee commends the design teamfor
  translating the visionary goal outlined in the
  Decadal Survey into a solid proof-of-principle
  concept
• The Committee believes that the Universities
  could prudently engage in the next phase of the
  CELT project, the preliminarydesign, technology
  and vendor development phase.

13
Two Studies, One Result

• Results from 2 x 2 years of studies
• It is feasible to build a 30m Telescope that will
  fulfill the science objectives of 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 GSMT
What the GSMT will do is learn the
physics of galaxy formation study the
birth of stars and planets seek new
biospheres
HST
Witnessing assembly of galactic masses
The physics of young Jupiter's
Gemini
x20
Log10 Fu (mJansky)
GSMT with Ex-AO
2.0
4.0
l (mm)
8.0
Witness planets forming
GSMT
30m telescope resolution and light gathering
power to analyze the physics of planets
galaxies
15
Comparative performance of a 30m GSMT with a
25m2 JWST
30m GSMT point design
Assuming a detected S/N of 10 for JWST on a
point source, with 6x5000s integration
GSMT advantage
NGST advantage
GSMT science strengths Angular resolution and
spectroscopy, the physics and dynamics of
galaxies, stars and young planets
16
CELT GSMT relative cost estimates

• Independently derived noticeable agreements
  and disagreements

lower
higher
agree
17
First Steps Toward a GSMT

• The committee recommends that technology
  development for GSMT begin immediately and that
  construction start within the decade.
• Astronomy and Astrophysics Survey Committee

18
Rapid Progress is Essential
We already have 2 x 2 years of studies completed,
A 2012 First Light requires a preliminary design
by 2006
19
Required GSMT Funding Profile
Cumulative Total 655M
Partners
NSF
NIO
A combination of public and private funds are
required to deliver a GSMT in the 2012-2013
timeframe
20
Conceptual Design Challenges for Next Generation
Telescopes
Committed cost vs. program life cycle
Early investment - reduces risk - maximizes
science Starting in FY04 essential to
completion early in JWST era
Common challenges for all ELT concepts Community
will have to work together to solve these
problems and to develop key technologies
Incurred cost
GSMT 2012-2014
10
JWST 2010-2012
70M initial investment - investigate high
risks and trade space
Conceptual design Optimize science
and mitigate technical risks in Public-Private
Partnership

• Quantify wind buffeting effects
• Active Adaptive
• controls design
• Optics fabrication feasibility
• Adaptive Optics
• Cost-performance trades

Private investment 35M
NSF investment 35M
FY04
FY05
FY06
21
Critical Elements of a Community-Based Design
Program

• Quantify wind buffeting effects
• Active Adaptive controls design
• Optics fabrication feasibility
• Adaptive Optics
• Cost-performance trades

Site characterization
Site prioritization
Year 1 Year 2 Year 3
Preliminary Design
integrated modeling
Wind buffeting models and CFD studies
System design
Active and adaptive simulation studies
Optical fabrication feasibility
Optics evaluation
End-to-end model infrastructure
Cost-performance trades
AO system models and simulation
AO System design
AO component development
layered control systems
active adaptive systems
wind flow
system response
22
ELTs require broad national and international
investment in key AO technologies
End of Investment
Start of Investment

• 4 technologies
• high risk
• High Power Lasers
• Deformable
• Mirrors
• Low noise Detectors
• System design

Next generation CCD detectors

• 4 technologies
• low /moderate
• risk
• High Power Lasers
• Deformable
• Mirrors
• Low noise Detectors
• System Design

Prototype Fiber Laser
Next generation DM
Xinetics, 12 clear aperture
MEMS 1 cm

• Encourage commercial product lines
• Estimated cost FY2004 through FY2010 65M

Investment now enables next generation and
spins-off to current generation of telescopes
30m GSMT/CELT
Full sky AO on current telescopes
Optical AO on 4ms
Planet finders on 8-10ms
23
Immediate Need Funding for Design Development
Phase

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

24
24
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 ELTs
• Sites
• Wind-buffeting
• Integrated modeling
• Instrument concepts
• Cost, schedule and management model

26
GSMT Science Working Group

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

27
GSMT SWG Members

• Chair Rolf-Peter Kudritzki, UH IfA
• SWG Members
• Jill Bechtold -- UA
• Mike Bolte -- UCSC
• Ray Carlberg -- U of T
• Matthew Colless -- ANU
• Irena Cruz-Gonzales -- UNAM
• Alan Dressler -- OCIW
• Betsy Gillespie -- UA

• Terry Herter -- Cornell
• Jonathan Lunine -- UA LPL
• Claire Max -- UCSC
• Chris McKee -- UCB
• Francois Rigaut -- Gemini
• Chuck Steidel -- CIT
• Doug Simons -- Gemini

Vice Chair Steve Strom NOAO
28
Driving Science Themes
GSMT

• The Birth of GalaxiesThe Archaeological Record
• Characterize Exo-Planets
• The Birth of Planetary Systems
• The Birth of Galaxies Witnessing the Process
  Directly
• The Birth of Large-Scale Structure

29
Science themes drive performance
GSMT

• For the majority of these themes, telescope
  aperture and image quality are key science
  drivers
• S/N a D2 D3
• Sensitivity (1/time) a D4 D6

Fully operational Adaptive Optics is a key
Science Requirement for ELTs
30
Top Performance Requirements
GSMT

• Near-diffraction limited performance over 2
  arc-minute fields
• High-dynamic-range imaging
• High sensitivity mid-IR spectroscopy
• Enhanced-seeing over 5 arc-minute field
• Wide-field, seeing-limited multi-object
  spectroscopy

31
GSMT SWG Next Steps

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

32
AURA New Initiatives Office
Management Board William Smith -- President of
AURA Jeremy Mould -- Director of NOAO Matt
Mountain -- Director of Gemini Observatory
Project Scientist Steve Strom
Program Manager Larry Stepp
System Scientist Brooke Gregory
Admin. Assistant Holly Novack
Clerk Jones - NOAO
Opto-Mechanical Myung Cho
Structures Paul Gillett
Controls George Angeli
Adaptive Optics TBD
Adaptive Optics Ellerbroek - Gemini
Optics Robert Upton
Software Development Anna Segurson
Structures Sheehan - Gemini
Mechanical Designer Rick Robles
Instruments Barden - NOAO
Sites Walker - NOAO
Fluid Dynamics Konstantinos Vogiatzis
Intern Int. Modeling SoonJo Chung
Intern Optomechanics Joon Pyo Lee
Intern Adapt. Optics Ahmadia - Gemini
Optical Fabrication Hansen - Gemini
33
Results of Point Design Studies

• Design studies established feasibility
• Design satisfies science requirements
• Telescope design accommodates needed instruments
• Technical challenges, but no show stoppers
• AO components
• Instrument components
• Wind buffeting
• Hierarchical control systems
• Cost estimate consistent with decadal survey

Identified technical challenges common to all ELT
concepts
34
GSMT Site Evaluation

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

35
Site characterization has started
Remote sensing
CFD Simulations
Weather stations
Turbulence MASS

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

36
Comparison of Chilean Sites
Site testing data available to all ELT Groups
37
Computational Fluid Dynamics

• Characterize wind flow to allow pre-selection of
  sites
• Wind intensity
• Turbulence characteristics
• Down-wind wakes
• NIO has recruited CFD modeling expert --
  Konstantinos Vogiatzis
• Characterization of Chilean sites well underway
• Analysis of other sites planned for 2nd Qtr 2003

Note Gemini South site location chosen using
only CFD analysis (CFD calibrated on
MK, measurements later confirmed CP choice)
38
Las Campanas Peak 2 Turbulent Kinetic Energy
CFD Tools available for any proposed ELT site
39
Integrated Modeling

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

An essential first step for this generation of
ELTs
40
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

Pressure sensors
Ultrasonic anemometer
41
Snapshot of Wind Pressure Resulting Mirror
Deformation
Measured Wind Pressure (Pascals)
Calculated Mirror Deformation on 30m

• Unique data set made available on web
• 116 five-minute test runs -- varying orientations
  and conditions
• Resource used by multiple ELT projects

42
Dynamic Structural Modeling
Preliminary 30m point design
Successfully used to design and verify
performance on Gemini
Dynamic model requires 10,000 nodes to determine
the effects of wind on an Extremely Large
Telescope structure
43
Adaptive Optics

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

44
AO SimulationCenter of M32
Davidge et al. (2000) 0.12 FWHM HK Gemini N
Hokupaa
Krist (1999) 8-m NGST PSF FWHM 0.032 J,
0.057 K Sampling 0.035 pixels
F. Rigaut GSMT PSF FWHM 0.009 J, 0.015 K
Sampling 0.005 pixels
45
AO Simulation Results
GSMT
NGST
AO/MCAO modeling tools and simulations available
to all ELT Groups (though you will need a
super-computer)
46
Integrated Model of science performance is the
result
NIO developing techniques, tools and experience
to assist multiple ELT programs
47
GSMT Instrument Studies
AURA and the community will have to work together
to develop new approaches for building 20M -
50M ELT Instruments
48
NIO Investments have already benefited the
Community

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

49

• We now have to take the next step

50
The Competition is now Global
Note Non-US Capital investment is x 3 that of
the US
The time has arrived for a national US consensus
on how to remain competitive on a global, not
parochial scale
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
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 DD Phase
• Building on point design studies

53
Laying the foundation for a new Public Private
Partnership
53
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

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
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
Embracing a New Paradigm

• The proposed partnership matches the AASC vision
• In addition toOWL, 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 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