Transcript Estimating the Costs of Extremely Large Telescopes

Update on LSST & GSMT
Jeremy Mould
Users Committee October 13, 2004
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GSMT SWG
The GSMT SWG is a community-based group convened to:
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Formulate a powerful science case for federal investment in GSMT
– Identify key science drivers
– Develop clear and compelling arguments for GSMT in the era of JWST/ALMA
– Discuss realization of key science as a function of design parameters: aperture,
FOV, PSF……
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Generate unified, coherent community support
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GSMT SWG Members
Chair: Rolf-Peter Kudritzki, UH IfA
SWG Members:
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Jill Bechtold -- UA
Mike Bolte -- UCSC
Ray Carlberg -- U of T
Matthew Colless -- ANU
Irena Cruz-Gonzales -- UNAM
Alan Dressler -- OCIW
Betsy Gillespie -- UA
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Terry Herter -- Cornell
Jonathan Lunine -- UA LPL
Claire Max -- UCSC
Chris McKee -- UCB
Francois Rigaut -- Gemini
Chuck Steidel -- CIT
Steve Strom -- NOAO
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TMT is a fusion of 3 concepts
GSMT
CELT
VLOT
The GSMT, CELT and VLOT point design telescope concepts.
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TMT Project FY2004
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Project Office established
Project manager appointed
Engineering efforts from 4 partners integrated to provide a 'reference
design'
– based on the heritage of the VLOT, CELT and GSMT efforts
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Moore funds in place for D and D Phase (gift to UC & Caltech)
CFI funds authorized
NSF proposal submitted
Key milestone: Baseline Design which will answer the following key design
issues/trades
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Is the elevation axis in front of or behind the primary?
Is the telescope optical configuration RC or AG?
What is the focal ratio of the primary ( f/1 – f/1.5)?
What final focal ratios should be provided ( f/15 – f/22)?
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Highest Priority Capabilities for
First Light
• diffraction-limited (10 mas @ 1.6m) imaging & spectroscopy
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0.8- to 2.5-micron wavelength
1-2 arcminutes multi-conjugate adaptive optics (MCAO) field
Strehl ratio at K-band of 0.7, constant across the field to 10%;
highly-multiplexed (~1,000 slits)
• seeing-limited 100 < R < 7,000 spectroscopy
– 0.32- to 1-micron wavelength range
– wide (10-20 arc-minute) field
• high-spectral-resolution (20,000 < R < 100,000) spectroscopy
– 1- to 5-micron
– 7- to 28-micron
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TMT phased implementation
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optical spectroscopy with 20,000 < R < 100,000
– 0.3 microns to 1 micron
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very high-contrast imaging near diffraction limit 1 to 2.5m
– contrast ratio > 108 at q > 4l/D from bright stars
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R ~3,000-5,000 spectroscopy
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fields ≥5 arcminutes
0.7- to 2.5-micron
sampling 0.15 arcseconds
image quality 80% enclosed energy in 0.3 arc-sec.
unit (IFU) heads or microslits
ground-layer adaptive optics system (GLAO);
mid-IR diffraction-limited imaging (Strehl > 0.5, 7m < l < 28m) over a
field >30 arcseconds;
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TMT AO modes
AO mode
Enables
Science
Mid-IR NGS AO
Diffraction limited
resolution l > M
Planet-forming
Environments
MCAO
Diffraction-limited
resolution in J, H, K
bands over 0.5-1’ fields
Galaxy Assembly;
deconstructing stellar
populations
MOAO
~0.1” resolution over 35’ fields for multi-object
spectroscopy
Young galaxy mass,
metallicity, & star
formation
ExAO
High dynamic range
imaging
Planet detection &
characterization
GLAO
0.2-3” resolution over 5- Galaxy evolution
10’ fields
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NIO
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provided 'point design' for GSMT -- key element of TMT planning
supports site testing (northern chile; Baja, CA; Hawaii); serves both theGMT
and TMT communities
interfaces with ESO to advance technologies of mutual interest
has contributed key technical and management leadership within TMT
post TMT project office, NIO will
– carry out two key TMT work packages (mid-IR Echelle; M2 assembly)
– continue site testing
– continue ESO collaborations (level TBD following allocation of TMT workpackages)
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GSMT vs JWST
Simulated monochromatic images of the ‘Antennae’
(local starburst galaxy: 105 seconds integration time)
Courtesy: Elizabeth Barton, GSMT SWG
GSMT
JWST
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GMT alternate
Magellan
partners +
Texas
7 x 8.4
meter
mirrors
Giant Magellan Telescope (GMT)
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OIR Planning
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Long Range Planning Committee (Chair: C. Pilachowski) is currently
working on a roadmap for large scale facilities
http://www.noao.edu/dir/lrplan/lrp-committee.html
• Where will the decision points be for public funding ?
• Look forward from 2005 as far as 2030.
– Two decadal surveys will occur before 2025, and these will
outrank this roadmap.
• The plan will show how present investments
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realize the new initiatives,
illustrate convergence paths,
lay the basis for facility closures and transfers,
and address community structural change.
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Overview and
Status
Opportunities
for Scientific
Participation
9 October 2004
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LSST Partners
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Project Technical Status
Systems Engineering – Requirements and Scope
~3 Gigapixel
Camera
8.4m 3-mirror
Telescope
Data Products &
Management
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Observing Simulator
• Initially Created By Abi
Saha
• New Simulation Tool in
Development
– K. Cook et. al.
– Foundation and Testbed
for Scheduler
A. Saha, NOAO
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The LSST Key Science
Drivers
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Nature of Dark Energy
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Solar System Map
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Observing Cadence
Absolute Astrometry – Link Vectors From Multiple Epochs
Optical Transients
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Image Quality – FWHM <0.8arcsec
Shape Systematics – PSF (e1,e2) < 0.0001
Observing Cadence
Data Processing – Real-Time Alerts (~30sec delay)
Galactic Structure
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Photometric Precision – 1% Internal, 2% Absolute
Astrometry
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Mapping the
Solar System:
Probing the
Fossil Record
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Mapping the
Galactic
Halo
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Weak Lensing and
Cosmology
• Cluster tomography
– Shear used to obtain mass maps
– Number density of clusters as function of redshift depends
on density fluctuations and distance scale
– Both depend on dark energy
• Strauss report
– Power spectrum, bispectrum, and shear cosmography
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Special
cadence to
go deeper?
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Evolving Optical Design
T3=3.25,
CC2=-0.5501
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Generator
Enclosure
(separate)
28 m D (92') dome
800 s.f.
Mechanical
Equipment
(interior)
Mechanical
Equipment
(exterior)
650 s.f.
750 s.f.
Observing Level 49'-0" (15 m)
Machine
Shop
Data
Processing
Room
Utility Level 33'-0"
Camera
Iinstrument
Shop
640 s.f.
3200 s.f.
860 s.f.
Receiving
820 s.f.
Base Level 0'-0"
W.C.
70 s.f.
Break
Room
190 s.f.
W.C.
70 s.f.
Control
Room
650 s.f.
Enclosure & Platform Lift Section
office
130 s.f.
office
130 s.f.
coating
chamber
mirror prep
area
office
130 s.f.
Work
Stations
(~8 people)
640 s.f.
office
130 s.f.
shop
storage
Summit Support Facility Plan
platform
lift
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v.
elex 6'
7'
Base Level Enclosure Plan
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30 ft.
5
10 m
J. Barr 12 Aug, '04
LSST Facilities
Conceptual Layout
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Wide – Deep - Fast
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~10 deg.2 per Field
~7m Effective Collecting Area
m~24th per 10 sec Exposure
Wide Coverage > 15,000 Square Degrees
Multiple Filters (e.g. bgriz´ - TBD)
~100+ Epochs in Each of >1500 Fields in Each Filter
Over Ten Years
• Accumulated Depth of 26th Magnitude in Each Filter
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Schedule & Milestones
First Light
2004 2005 2006 2007 2008 2009 2010 2011 2012 2013
CoDR
PDR
CDR
Design
Order glass
Construction
Start final
camera fab
Optics on
site
Integration
First Light
Commissioning
Operation
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Camera
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Focal Plane Array
– 10 mm pixels  0.2 arcsecond/pixel (~1/3 seeing-limited PSF)
– 64 cm diameter  10 square degree FOV
 3 Gpixels
– Integrated front-end electronics
– 16 bits/pixel, 2 sec readout time  3 GB/sec
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 Parallel readout
Housing / Filters / Optics / Mechanisms
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Primary Mirror Contract
• Private Donor Committed to Buy LSST Mirror
– University of Arizona Borosilicate Cast Mirror
– Similar to LBT Primary with Very Large Hole
• Contract Approved
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Materials and Engineering
Casting
Optical Figuring
Cell Integration and Testing
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Telescope Structure
• Initial Warren Davidson Study Complete
– Long Tube
– Stiff Structure, f(n1)=10hz
– Relatively Light , 200T
• Preparing for Second Study
– Short Tube
– Open Structure
– Industrial Source
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Site Selection
• First Down-Selection Completed in May 2004
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Cerro Pachon
Las Campanas
San Pedro Martir
La Palma
• Study to Evaluate Satellite Data Issues
• Correlating Local Data to Global Weather Patterns
• Final Site (2) Selection Meeting 14 January 2005
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Summary
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LSST Corporation is Established
The Mission is Solidifying
Management Organized & Vision is Clear
Project Teams Developing
Technical Advancement Accelerating
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