TMT Project Status
C. Steidel, for the TMT Project
GSMT SWG Meeting
Los Angeles
October 20, 2005
1
Contents
Current Design Baseline
Instruments and adaptive optics systems
Capabilities and their connection to the GSMT-SWG
report
Operations models and US community access
Schedule
2
The TMT Partnership
TMT follows the NAS Decadal Survey recommendation
that a public-private partnership is the best way to build &
operate a US-led 30-m telescope
Current partners (for Design and Development Phase)
are:
–
–
–
–
University of California
Caltech
ACURA (Canada)
AURA (NSF)
Although partners are currently “equal”, ultimate shares
(e.g. of observing time) will be based on contributions to
capital & operations.
3
TMT Precursor Studies
TMT follows from a careful consideration of three,
independently-conceived & independently-reviewed,
point designs representing $6M total effort
CELT (UC+Caltech)
VLOT (Canada)
GSMT (NOAO/Gemini)
– Broad exploration of technical options
– Positive reviews by outside reviewers
– TMT consolidates the best aspects of these designs
– Single reference design now established by the Project
4
TMT Overall Structure
TMT governance established in June 2003
– Agreements between the partners
– Formation of Science Advisory Committee
equal membership/representation from each of the 4 partners
– Formation of Board of Directors
– Appointment of Project Manager, Gary Sanders (Apr 2004)
Development Phases
– Design Development Phase (2004-2008)
$35M secured from G&B Moore Foundation (Caltech/UC)
$17.5M from each of Canada and AURA (NSF)
– Construction phase (2009 – 2014)
– Science Operations (2015 - )
(Assuming timely delivery of capital & operational resources)
5
Distributed Project Effort
TMT Project Headquarters- Pasadena : 32 FTE
ACURA/AURA/UC/Caltech : ~35 FTE
Instrument teams, industry design teams: additional ~50
participants
– major industry design teams include: AMEC, SAGEM, ITT, Zygo,
Cilas, tOSC, Hytec, Night Sky
6
The Project Ahead, First Light and the
First Decade of TMT Science
The TMT Science Advisory Committee (SAC) has
provided a Science Requirements Document (SRD)
– It presents a vision of the first decade of TMT
– Most of the effort will be to realize the foundation for this decade,
reaching first light era science
Design and Development Phase (DDP) – (2004 – 2008)
Construction Phase – (2009 – 2014)
Early Operations Phase – (2012 – 2016)
Operations Phase – (2016 – 2024)
7
The Project, The Science, The Systems
Design Development Phase (DDP) budget and schedule defined
Project office established in Pasadena
Project organization in place for DDP
– Partnership teams
– Instrument partners
– Industrial partners
Science Requirements Document (SRD) delivered and guiding DDP
Detailed Science Case under continuing development (currently a
90-page document)
Science Advisory Committee (SAC) in intimate dialog with project
DDP activities
Systems studies mounting
Systems engineering processes developing
Operational scenarios discussion is started
8
TMT Reference Design
30m filled aperture, highly segmented
Aplanatic Gregorian (AG) two mirror
telescope
f/1 primary
f/15 final focus
Field of view 20 arcmin
Elevation axis in front of the primary
Wavelength coverage 0.31 – 28 µm
Operational zenith angle range 1° thru 65°
Instruments (and their associated AO
systems) are located on large Nasmyth
platforms, addressed by an articulated
tertiary mirror.
Both seeing-limited and adaptive optics
observing modes
AO system requirements and architecture
defined
First generation instrument requirements
defined
9
30m Primary Mirror Concept
738  1.2m segments
each 0.040m thick
10
TMT Reference Design
11
M2 System Overview
M2 system
Two interchangeable assemblies:
CM2 & AM2
CM2 - “Conventional” M2
•
Seeing limited performance
•
Used for commissioning
•
Initial operations
•
Will be replaced by AM2
•
Kept as maintenance spare
AM2 - Adaptive M2
• Full AO capability
• Developed under separate
study (SAGEM)
12
M3 System Overview
M3 system
Mirror
• 4.11 x 2.91m flat to cover
20 arcmin fov
• Meniscus glass or glass
ceramic substrate
M3 cell
• High stability
active/passive supports
Positioner
• Rotates to switch beam to
Nasmyth instruments
• Active tracking to steer
beam onto instrument
13
SRD Science Instruments
Adaptive Optic systems defined
– NFIRAOS (Narrow Field facility AO system) for first light
– MOAO (“Multi-Object Adaptive Optics” ~20 positionable, 5”
compensated patches in 5’ adressable field)
– MIRAO (MidIR AO)
– MCAO (wide field AO, optimized for photometric and astrometric goals)
Eight Instruments identified
– IRIS, a NIR imager and integral field spectrograph working at the
diffraction limit, 0.8-2.5 microns; fed by NFIRAOS
– WFOS, a wide field, seeing-limited optical spectrograph (possibly
GLAO-compensated)
– IRMOS, a NIR multi-object integral field spectrograph fed by MOAO
– MIRES, a mid-IR high resolution echelle spectrograph fed by MIRAO
– PFI, a “planet formation instrument”, which combines a high contrast AO
system and an imaging spectrograph.
– NIRES, a NIR echelle spectrograph, also fed by NFIRAOS
– HROS, a high spectral resolution optical echelle spectrograph
14
– WIRC, a wide field NIR camera fed by multi-conjugate AO
IRIS
Infrared Imaging Spectrograph
Integral Field Spectrograph and Imager working at the diffraction limit
Wavelength range: 0.8-2.5µm; goal 0.6-5µm
Field of view: < 2 arcsec for IFU, up to 10” for imaging mode
Spatial sampling: 0.004 arcsec per pixel (Nyquist sampled (/2D)) over 4096 pixels for
IFU); over 10x10 arcsec for imaging
–
–
Plate scale adjustable 0.004, 0.009, 0.022, 0.050 arcsec/pixel
128x128 spatial pixels with small ( ≤ 0.05) wavelength coverage
Spectral resolution
–
–
R=4000 over entire Y,J, H, K,( L) bands, one band at a time
R=2-50 for imaging mode
Low background (increase inter-OH sky + tel by no more than 15%)
Detector: Dark current and read noise ≤ 5% of background for t=2000s
Throughput: as high as practical
Parallel imaging: goal
15
WFOS
Wide Field Optical Spectrograph
–
–
–
–
–
–
–
–
–
–
Multi-object spectroscopy over as much of 20’ field as possible
Wavelength range: 0.31-1.1µm (0.31-1.6µm goal). ADC required
Field of view: 75 arcmin2 ; goal: 300 arcmin2
Total slit length ≥ 500 arcsec
Image quality: ≤ 0.2 arcsec FWHM over any 0.1µm
Spatial sampling: ≤0.15 arcsec per pixel, goal ≤ 0.10 arcsec
Spectral resolution: R=5-5000 for 0.75” slit; goal: 150-6000
Throughput: ≥ 30%
Sensitivity: photon noise limited for all exposures > 60s
Background subtraction systematics must be negligible compared to photon
noise for total exposure times as long as 100 Ks
– Stability: Flexure < 0.1 pixel at the detector is required
– Desired: cross dispersed mode, IFU option, narrow band imaging, enhanced
image quality using adaptive optics (GLA0)
GLA0 trade study completed
16
IRMOS
Infrared Multi-Object Spectrograph
MOAO/Deployable IFU spectrometer
0.8-2.5µm
FoV: IFU heads deployable over 5 arcmin field
Wavefront quality: preserve that delivered by AO system
Image quality: diffraction-limited images, tip-tilt ≤0.015 arcsec rms
Spatial sampling
– 0.05x0.05 arcsec pixels, IFU head 2.0 arcsec, ≥ 10 IF units
Spectral resolution
– R=2000-10000 over entire J, H, K bands, one band at a time
– R=2-50 for imaging mode
Low background (increase inter-OH sky + tel by no more than 15%)
Detector
– Dark current and read noise ≤ 5% of background for t=2000s
Throughput: as high as practical
17
MIRES
Mid-IR Echelle Spectrometer
Mid-IR Diffraction Limited Spectrometer
8-18µm, 5-28µm goal
FoV 10 arcsec
Slit length: 3 arcsec order separation, or IFU
Wavefront quality: preserve that delivered by AO system
Image quality: diffraction-limited images, limited by AO
Spatial sampling
–
0.017x0.017 arcsec pixels
Spectral resolution
–
–
5000< R <100000 with diffraction-limited slit
R=2-50 for imaging mode
Low background (increase natural sky + tel by no more than 15%)
Detector
–
2k x 2k
Throughput: as high as practical
Chopping and nodding as needed
18
PFI
Planet Formation Imager
1-2.5µm, goal 1-5µm
Field of view 0.03-1 arcsec radius
Image quality/contrast
– Detect planet at 106 contrast or 107 goal for 1st generation
system
– Suitable coronagraph
– Optical system should not preclude 108 contrast in H band for
R<8 mag
Critically sampled at 1µm (0.0035 arcsec pixels)
Spectral resolution ≤ 100
19
NIRES
Near IR Echelle Spectrometer
Wavelength range: 1-5µm, simultaneous 1-2.4µm, 3.5-5µm
Field of view of acquisition camera: 10 arcsec, 0.0035 arcsec/pixel
Slit length: 2 arcsec
Image quality: diffraction limited
Spatial sampling: Nyquist sampled (/2D)
Spectral resolution: 20,000<R<100,000
Low background (increase natural sky + tel by no more than 15%)
Detector: Dark current and read noise ≤ 5% of background for
t=2000s
High throughput
20
HROS
High Resolution Optical Spectrometer
Seeing limited optical spectrometer
Wavelength range: 0.31-1µm (0.3-1.3µm goal)
Field of view: 10 arcsec
Total slit length 5 arcsec, separation between orders
Image quality: ≤ 0.15 arcsec rms
Spatial sampling: ≤ 0.2 arcsec per pixel
Spectral resolution: R=50,000 for 1 arcsec slit,
R=90,000 with slicer
Throughput: ≥ 30% telescope focal plane to detected
photons
21
WIRC
Wide-field Infrared Camera
Precision photometry and astrometry instrument
Wavelength range: 0.8-5µm, goal 0.6-5µm
Field of view: 30 arcsec, contiguous
Image quality: diffraction limited as delivered by AO
Spatial sampling: Nyquist sampled (/2D)
Spectral resolution: R=5-100 with filters
22
AO Systems
TMT is designed for high-performance (120nm wavefront error) AO
from the beginning
Adaptive Optic systems defined in SRD
– NFIRAOS (Narrow Field facility AO system) for first light
2’ “technical field”, upgrades to wide field system.
– MOAO (“Multi-Object Adaptive Optics” ~20 positionable, 5
compensated patches in 5 technical field)
– MIRAO (MidIR AO, optimized for low emissivity in mid-IR)
– MCAO (wide field AO, optimized for photometric and astrometric goals)
Significant effort during DDP to define AO systems, component risks
and global image quality error budget for telescope-AO-instrument
systems.
23
First Light AO Capabilities
NFIRAOS (Narrow-Field IR AO System)
–
–
–
–
–
–
Facility AO system for IRIS (and eventually NIRES and WIRC)
150-200 nm RMS WFE as initially implemented
50% sky coverage at the galactic pole
30 arc sec compensated FOV
cooled optical system to minimize background in K band
Implied component and design parameters:
Order 60x60 wavefront sensing and correction
5-9 LGS WFS (with ~17W of laser power per beacon)
MCAO system with 2 DMs conjugate to 0 and 10-12 km
Near IR NGS tip/tilt/focus sensing with 2’ diameter guide field
MIRAO (option)
– 7-20 mm (goal 3-20 mm) spectral band, 10” field of view
– 1 (3) LGS, 1 tip/tilt/focus near IR NGS WFS
– Order 15x15 (30x30) DM (requires 3 additional warm surfaces)
24
Instrument Deployment Concept
25
Instrument Design Feasibility Studies
•9 instrument feasibility
studies funded via open
competition
- Feb 2006 completion
- Feedback to telescope, AO and
operations requirements
- Develop instrument concepts
- Extended Science Case via
associated science teams -- wide
community participation
•major presence at upcoming
SPIE expected from all of these
studies
(U. Colorado HROS concept)
26
TMT AO Development Program
DDP program addresses TMT AO architecture, design
and technology development
Key technologies and demonstrations
–
–
–
–
–
–
–
MEMS
Lasers
Infrared tip-tilt wavefront sensing
Open loop control
Tomography
Wavefront sensor
Adaptive secondary technology
27
TMT Experience with Adaptive Optics
UC Lick
Gemini
CFHT
Palomar
Keck
28
Adaptive Optics has come of age!
Ghez (UCLA) & collaborators
Gemini Hokupa’a/QUIRC image of
Galactic Center. Expanded view
shows IRS 13E & W in Kp
40 x 40 arcsecond mosaic, colorcomposite NIRC2 image (at ~2.2 um)
of the Galactic Center using Keck Laser
29
Keck AO Imaging of Uranus
Courtesy: L. Sromovsky
30
NFIRAOS side view
Science
Laser
Natural
31
Optical Design of LGS
WFS
SH WFS
6 Copies
Wavefront Error
1.4x spec
Zoom
DM/WFS
Distortion
3x spec
(Map scale
100x)
32
Subsystem
Decomposition
33
GSMT SWG Science Case
The goals/capabilities of TMT are very well aligned with
those of the GSMT SWG
1First
light and the early
assembly of galaxies
IRIS, IRMOS, WFOS
The discovery and
characterization of extrasolar planets
PFI, HROS, NIRES, IRIS
Stellar Populations in the
Local Universe: formation
and evolution of galaxies
IRIS, HROS, WIRC
Tomographic surveys at z>2
WFOS
1 GSMT
high-level goals from “Frontier Science Enabled by a GSMT” SWG report 7.2.03
34
TMT Instrument Summary
Instrument
Near-IR DL Spectrometer &
Imager (IRIS)
Spectral
Resolution
≤4000
Wide-field Optical
Spectrometer (WFOS)
300 - 5000
Multi-IFU, near-DL, near-IR
Spectrometer (IRMOS)
2000 - 10000
Example Science Cases
• Assembly of galaxies at large redshift
• Black holes/AGN/Galactic Center
• Resolved stellar populations in crowded fields
• IGM structure and composition 2<z<6
• High-quality spectra of z>1.5 galaxies suitable for measuring stellar pops,
chemistry, energetics
• Near-IR spectroscopic diagnostics of the faintest objects
Mid-IR Echelle Spectrometer &
Imager
5000 - 100000
ExAO I
(PFI)
50 - 300
Optical Echelle (HROS)
30000 - 50000
MCAO imager (WIRC)
5 - 100
Near-IR, DL Echelle (NIRES)
5000 - 30000
• JWST followup
•Galaxy assembly, chemistry, kinematics during the “epoch of Galaxy Formation”
• Physical structure and kinematics of protostellar envelopes
• Physical diagnostics of circumstellar/protoplanetary disks: where and when
planets form during the accretion phase
• Direct detection and spectroscopic characterization of extra-solar planets
• Stellar abundance studies throughout the Local Group
• ISM abundances/kinematics
• IGM characterization to z~6
• Galactic center astrometry; general precision astrometry
• Stellar populations to 10Mpc
• Precision radial velocities of M-stars and detection of low-mass planets
• IGM characterizations for z>5.5
Site Testing
An effort of the TMT Project Site team, CTIO, NIO,
UNAM, UofH, Gemini, CFHT, HIA
Robotic data collection underway at 2 sites in Chile
(Tolar, Armazones), San Pedro Martir (Mexico), and
Mauna Kea; two more Chilean sites in process.
– high altitude sites (>4000m) in both hemispheres included
The most comprehensive (and ambitious) astronomical
site survey work ever
Site Requirements Document has been authored and is
under review
– Includes data evaluation/figure of merit strategy
36
Site Testing: Instruments & Parameters
Weather stations
DIMM – seeing monitors
MASS – turbulence profilers
SODAR – acoustic sounders
IRMA – mid-infrared radiometers
ASCA – Allsky cameras
Particle sensors
Sonic anemometers
Simulations, satellite analysis
–
–
–
–
–
–
–
–
temp, hum, wind, press, sol.rad, heat flux
seeing, coh. time, basic photometry
high-el. profiles, isopl. angle, coh. time
20 – 800m turb/wind profiles, coh.time
PWV, atm. transparency
Cloud statistics (incl. cirrus), light pollution
Ground level dust particle count
7m wind, temperature, turbulence
– Turbulence, weather, long baseline
Other considerations:
– Location, elevation, geology, access, cost of construction and operation,
operation model, ...
37
DDP Instrumentation Plan
38
Construction phase
39
Telescope Optics Status
An effort of TMT Project, UCSC, UCI, NIO, industrial
partners SAGEM, Zygo, ITT/Tinsley, Hytec
Telescope requirements and error budget development is
supporting optics design efforts
M1 segment polishing awards initiated (Zygo, SAGEM,
ITT/Tinsley)
– Segments must be produced at lowest possible cost
M1 Segment Assembly design underway with Hytec Inc. of
Los Alamos
M2 (secondary), M3 (tertiary) designs well underway
40
Telescope Structure Status
An effort of TMT Project Office, HIA and AMEC
Reference Design studied and dissected by AMEC
– Design strengths, weaknesses studied and points of departure
for next design phase are identified
Methods and infrastructure for assessing structure
performance (finite element analysis (FEA), merit
function routines (MFR)) are being implemented
Work on requirements and interfaces accelerating
41
Telescope Controls Status
Actuator and edge sensor studies underway
– Studies of humidity sensitivity of Keck edge sensors by TMT
underway at Keck
– Edge sensor design study underway with LBL group that worked
on Keck design
Alignment and Phasing System design underway with
UCI group that designed Keck system
42
AO/Science Instruments Status
All feasibility studies underway for WFOS, IRIS, MIRES,
PFI, HROS, IRMOS
NFIRAOS design well underway by TMT Project and HIA
group
SAGEM adaptive secondary contract underway
CILAS piezo deformable mirror contract underway
Laser Guidestar Facility design underway with NOAO group
Laser development following Gemini/Keck program
Real Time Controller design study with tOSC
UVic woofer/tweeter experiment underway
Palomar Multiple Guidestar experiment underway
AOWG/IWG and weekly design coordination meetings are
quite effective
43
Enclosure Status
An effort of HIA, AMEC, NIO, TMT Project Office
Successful 6 month design review conducted July 8
Enclosure Requirements Document under version
control
Design effort had been comparing 4 configurations
– Downselect to 2 on July 8
– Downselect to 1 at 9 month review
In fact, July 8 review resulted in tentative downselect to
one configuration
– Calotte selected due to lower mass, lower cost, though
technically novel
– Carousel carried for 3 months as conventional backup
44
Enclosure Structural Optimization
Calotte
Dome-Shutter
Carousel
Aperture ring at
Zenith=0 deg
Co-Rotating
Co-Rotating (showing
internal
frame)
Aperture ring
at
Zenith=65 deg
45
Summit/Support Facilities Status
Facilities requirements review August 9, 2005
Facilities Requirements and site dependence discussed
extensively at Aspen (Sep 2005) “TMT Week” meeting
– The arrangement of summit and support facilities is strongly
dependent on sites
Goal is to transition to Architect/Engineer studies this
year
Operations strategy impacts requirements
– Site Selection requirements document provides initial discussion
– Observatory Scientist David Silva will lead study of this area
46
Operations & Development
Operations and development
– Assume $40M/yr for operations
– Assume $20M/yr for development
Possible sources of operational funds ($40M/yr)
– UC+Caltech 25%, Canada 25%, NSF 50%
Operations style
–
–
–
–
We will support traditional astronomer-led observing
We will support queue or service observing
Mix will be set by maximizing scientific productivity
Data will be archived and available to all after proprietary period
Purpose of Development funds
–
–
–
–
New instruments
Instrument upgrades
AO upgrades and new AO capabilities
Facility upgrades including guiders, etc
47
Observing Time
If we use current projected partner contributions, we
might expect observing time to be distributed very
roughly as:
– Private
– US Community through AURA
– Canada
25-50%
50-25%
25%
Actual distribution will depend on financial contributions
of the partners.
48
Operations Planning
Lead role taken by Observatory Scientist
– David Silva (ESO/VLT) is joining TMT to assume this role
Project Scientist and SAC will play a major role
Operations Advisory Group will be formed as soon as the
Observatory Scientist is on board
– Group will represent the 4 partners and the operational expertise
of Keck, Gemini and VLT
Already can see operational questions arising in all
design discussions
49
Key Dates in the DDP
TMT Week (Sept 26 – 30, 2005; Aspen Center for
Physics)
– Mid-point review of all subsystems
Conceptual Design Review (CoDR) (May 8 – 11, 2006)
Cost Review (Sept 25 – 29, 2006)
– Update CoDR all subsystems
– Cost review for project scope decisions by TMT Board
PDR/Construction Proposal Review (Sept 24 – 28, 2007)
– Update CoDR to PDR for critical systems
– Definitive cost/scope, reference schedule
50
Construction Phase
Approval to start ($$ available)
Primary mirror detail design review
Site Development FDR
Complete enclosure
Complete telescope installation
Begin segment installation
First light with 1/4 segments
All segments installed, phased
Begin TMT science
Jan 2008
Apr 2008
Apr 2008
Feb 2012
Oct 2012
Aug 2012
Jul 2013
Apr 2014
Jan 2015
51
Major Construction Phase Milestones
Construction initiated Q1CY2009
Site Specific Designs/Site Mobilization Q4CY2008
Site facilities/enclosure accepted – Q2CY2012
Initial instrument installed – Q1CY2014
Additional First Light Instruments delivered – CY2014
First Light, all segments phased – Q2CY2014
First science, initial instrument – Q1CY2015
52
A Vision of TMT – AAS Calendar 2006
53
200 Inch and TMT
54
END
55