nio gsmt overview vlot/gsmt workshop victoria, bc 17 july, 2001 s. strom, l. stepp
TRANSCRIPT
NIO GSMT Overview
VLOT/GSMT WORKSHOP
Victoria, BC
17 JULY, 2001
S. Strom, L. Stepp
AURA NIO: Mission
• In response to AASC call for a GSMT, AURA formed a New Initiatives Office (NIO)
– collaborative effort between NOAO and Gemini to explore design concepts for a GSMT
• NIO mission
“ to ensure broad astronomy community access to a 30m telescope contemporary in time with ALMA and NGST, by playing a key role in scientific and technical studies leading to the creation of a GSMT.”
Goals of the NIO• Foster community interaction on GSMT
• Develop point design
• Conduct studies of key technical issues and relationship to science drivers
• Optimize community resources:– explore design options that yield cost savings, – emphasize studies that benefit multiple programs, – collaborate to ensure complementary efforts, – give preference to technologies that are extensible
to even more ambitious projects.
AURA New Initiatives Office
E n g in eerin g O vers ig h tJ im O sch m an n
P ro jec t S c ien tis tS teve S trom
C on trac ted s tu d ies P art t im e su p p ortN O A O & G em in i**
A d m in is tra tive A ss is tan tJen n ife r P u rce ll
O p to -M ech an icsM yu n g C h o
C on tro lsG eorg e A n g e li
A d ap tive O p tic sE lle rb roek /R ig au t
In s tru m en tsS am B ard en
M ech an ica l D es ig n erR ick R ob les
S tru c tu resP au l G ille tt
S ite Tes tin gA lis ta ir W a lke r
P rog ram M an ag erL arry S tep p
S ys tem s S c ien tis tB rooke G reg ory
M an ag em en t B oardM att M ou n ta inJerem y M ou ldW illiam S m ith
Comparative performance of a 30m GSMT with a 6.5m NGST
1 101E-3
0.01
0.1
1
10
Comparative performance of a 30m GSTM with a 6.5m NGST
S/N
Ga
in (
GS
MT
/ N
GS
T)
Wavelength (microns)
R=5 R=1,000 R=10,000
Assuming a detected S/N of 10 for NGST on a point source, with 4x1000s integration
GS
MT
a
dv
an
tag
eN
GS
T a
dva
nta
ge
R = 10,000 R = 1,000 R = 5
GSMT/NGST at High Spectral Resolution
1 10
0.01
0.1
1
10
17.0
12.3
4.6
Molecular line spectroscopy S/N = 100
S/N
Gai
n (
GS
MT
/ N
GS
T)
Wavelength (microns)
R=10,000 R=30,000 R=100,000
Developing Science Cases• Two community workshops (1998-1999)
– Broad participation; wide-ranging input
• Tucson task group meetings (SEP 2000)– Large-scale structure; galaxy assembly
– Stellar populations
– Star and planet formation
• NIO working groups (MAR 01 – SEP 01)– Develop quantitative cases; simulations
• NIO-funded community task groups (CY 2002)
• NIO-funded community workshop (CY 2002)– Define “Science Reference Mission”
KEY SCIENCE ENABLED BY GSMT
Origin of structure in the universe: from the big bang to planetary systems
Najita et al (2000,2001)
Tomography of the Universe• Goals:
Map out large scale structure for z > 3Link emerging distribution of gas; galaxies to CMB
• Measurements:Spectra for 106 galaxies (R ~ 2000)Spectra of 105 QSOs (R ~15000)
• Key requirements:20’ FOV; >1000 fibers
• Time to complete study with GSMT: 3 years• Issues
– Refine understanding of sample size requirements– Spectrograph design
Mass Tomography of the Universe
z~0.5
Existing Surveys + Sloan
z~3
Hints of Structure at z=3(small area)
100Mpc (5Ox5O), 27AB mag (L* z=9), dense samplingGSMT 1.5 yrGemini 50 yrNGST 140 yr
Tomography of Galaxies and Pre-Galactic Fragments
• Goals:Determine gas and stellar kinematicsQuantify SFR and chemical composition
• Measurements:Spectroscopy of H II complexes and underlying stars
• Key requirements:Deployable IFUs feeding R ~ 10000 spectrographWide FOV to efficiently sample multiple systems
• Time to complete study with GSMT: ~1 year• Issues
– Modeling surface brightness distribution– Understanding optimal IFU ‘pixel’ size
Tomography of Individual Galaxies out to z ~3
• Determine the gas and stellar dynamics within individual galaxies• Quantify variations in star formation rate– Tool: IFU spectra [R ~ 5,000 – 10,000]
GSMT 3 hour, 3 limit at R=5,000
0.1”x0.1” IFU pixel(sub-kpc scale structures)
J H K 26.5 25.5 24.0
Origins of Planetary Systems• Goals:
– Understand where and when planets form– Infer planetary architectures via observation of ‘gaps’
• Measurements:Spectra of 103 accreting PMS stars (R~105; )
• Key requirements:On axis, high Strehl AO; low emissivity
• Time to complete study with GSMT:2 years
• IssuesUnderstand efficacy of molecular ‘tracers’Trades among emissivity; sites; telescope & AO design
Probing Planet Formation with High Resolution Infrared Spectroscopy
Planet formation studies in the infrared (5-30µm):
Probe forming planets in inner disk regions Residual gas in cleared region low emission Rotation separates disk radii in velocity High spectral resolution high spatial resolution
8-10m telescopes with high resolution (R~100,000) spectrographs can detect the formation of Jupiter-mass planets in disks around nearby stars (d~100pc).
S/N=100, R=100,000, >4m
Gemini out to 0.2kpc sample ~ 10s
GSMT 1.5kpc ~100s
NGST X
Stellar Populations• Goals:
Quantify IMF in different environmentsQuantify ages; [Fe/H]; for stars in nearby galaxiesDevelop understanding of galaxy assembly process
• Measurements:Spectra of ~ 105 stars in rich, forming clusters (R ~ 1000)CMDs for selected areas in local group galaxies
• Key requirements:MCAO delivering 2’ FOV; MCAO-fed NIR spectrograph
• Time to complete study with GSMT: 3 years• Issues
– MCAO performance in crowded fields
GSMT System Considerations
Science Mission- DRM’s
GSMTConcept
(Phase A)
Support &Fabrication
Issues
Active Optics (aO)
SiteCharacteristics
Enclosureprotection
Adaptive Optics
Instruments Full SystemAnalysis
NIO Approach
Parallel efforts
– Address challenges common to all ELTs
• Wind-loading
• Adaptive optics
• Site
– Explore point design
• Start from a strawman
• Understand key technical issues
Enemies Common to all ELTs
Wind…..
The Atmosphere……
Wind Loading
Primary challenge may be wind buffeting– More critical than for existing telescopes
• Structural resonances closer to peak wind power• Wind may limit performance more than local seeing
Solutions include:– Site selection for low wind speed– Optimizing enclosure design– Dynamic compensation
• Adaptive Optics• Active structural damping
0 50 100 150 200 250 300-2
-1.5
-1
-0.5
0
0.5
1
1.5
Time History: time (second)
pres
sure
(N
/m2)
AVERAGE Pressure (C00030oo)
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
AnimationWind pressure: C00030oo
test_2, day_2, Azimuth angle=00, Zenith angle=30, wind_gate:open, open; wind speed=11 m/s
Wind Pressure Structure Function C00030oo
0 1000 2000 3000 4000 5000 6000 7000 80000
0.5
1
1.5
2
2.5
3
3.5
4
sensor spacing, d (mm)
RM
S p
ress
ure,
Prm
s (N
/m2)
Average Structural Function for C00030oo
Prms = 0.076124 d ** 0.4389
How to scale to 30 meters:
D(d) = 0.076 d 0.43
0 1000 2000 3000 4000 5000 6000 7000 80000
0.5
1
1.5
2
2.5
3
3.5
4
sensor spacing, d (mm)
RM
S p
ress
ure,
Prm
s (N
/m2)
Average Structural Function for C00030oo
Prms = 0.076124 d ** 0.4389
30M
RMS pressure differences
Spatial scale
The Gemini South wind test results
are available on the NIO Web site at:
www.aura-nio.noao.edu
AO Technology Constraints: DMs and Computing power
(50m telescope; on axis)
r0(550 nm) = 10cm No. of Computer CCD pixel Actuator pitch S(550nm) S(1.65m) actuators power rate/sensor
(Gflops) (M pixel/s)
10cm 74% 97% 200,000 9 x 105 800
25cm 25% 86% 30,000 2 x 104 125
50cm 2% 61% 8,000 1,500 31 SOR (achieved) 789 ~ 2 4 x 4.5
Early 21st Century technology will keep AO confined to > 1.0mfor telescopes with D ~ 30m – 50m
AO Technology Constraints:Guide stars and optical quality
MCAO system analysis by Rigaut & Ellerbroek (2000):• 30 m telescope• 2 arcmin field• 9 Sodium laser constellation 10 watts each• 4 tip/tilt stars (1 x 17, 3 x 20 Rmag)• Telescope residual errors ~ 100 nm rms• Instrument residual errors ~ 70 nm rms
System performance:(m) Delivered Strehl
1.25 0.2 ~ 0.4 1.65 0.4 ~ 0.6
2.20 0.6 ~ 0.8
PSF variations < 1% across FOV
Site Evaluation ELT site evaluation more demanding Evaluation criteria include
– surface and high altitude winds
– turbulence profiles
– transmission
– available clear nights (long-term averages)
– cirrus cover (artificial guide star performance)
– light pollution
– accessibility
– available local infrastructure
– land ownership issues
Site Evaluation
NIO gathering uniform data for sites in:– Northern Chile – Mexico and Southwest US– Hawaii
Point Design: Philosophy
Select plausible design that addresses key science requirements
Identify key technical challenges Focus analysis on key challenges Evaluate strengths and weaknesses
– guide initial cost-performance evaluation– inform concept design trades
Point design is only a strawman!
Point Design: Motivations
Provide a practical basis for wide-field, native seeing-limited instruments– science drivers strong
Explore a radio telescope approach– possible structural advantages
• elevation bearing size comparable to primary– possible advantages in accommodating large
instruments
Point Design: End-to End Approach
• Science Requirements (including instruments)• Error Budget• Control systems• Enclosure concept
– Interaction with site, telescope and budget
• Telescope structure– Interaction with wind, optics and instruments
• Optics– Interaction with telescope, aO/AO systems and instruments
• AO/MCAO – Interaction with telescope, optics, and instruments
• Instruments– Interaction with AO and Observing Model
Derived Top Level Requirements
Narrow field AO 1 2 3 MCAO 1 2 3 Low order AO 1 2 3 Seeing limited (PF) 1 2 3Field of View 10 arcsec + - + 2 arcmin + + 2 arcmin + 20 arcminPrinciple wavelegths 1.0 - 2.5 microns 1.0 - 2.5 microns 1.0 - 20 microns 0.4 - 2.5 micronsPSF
Resolution Diffraction limited + + Diffraction limited + 0.1-0.2 arcsec + 0.4-0.7 arcsec +Stability 1% + 5% - - 2% 2%
Strehl 80% 50% <10% 0%Photom. accuracy(derived) 1% 5% - - 2% 1%
Astrometric accuracy 10 -̂4 arcsec + + 10 -̂3 arcsec - 10 -̂2 arcsec 0.05 arcsecStability timescale 3,600 s 3,600s 3,600s 10,000 sEmissivity <20% - <20% 10% 15%Maintenance/Ops <15% <15% <15% <15%Reliability 90% 90% 90% 90%Science Efficiency 90% 90% 90% 90%
1 Galaxy Evolution and LS Structure2 Stellar Populations3 Star and Planet Formation
Key:+ meets needs- does not meet needs
irrelevant or not critical
How to r ead this table:
Four telescope “Operating regimes” are defined and the specs for thetelesc ope (not the instrument) in each regime are cited. There are columns atthe right of each regime labeled 1,2,3 for the th ree science programsdiscussed in the NO AO panel W orkshop. In these columns the spe cs areassessed in term s of the adequacy for each sc ience program .
Matt:I think this mode is important, its our only "thermal IR" mode, and we may find some spectroscopy modes are so photon starved they
30m Giant Segmented Mirror Telescope Point Design Concept
Typical 'raft', 7 mirrors per raft
Special raft - 6 places, 4 mirrors per raft
1.152 m mirror across flats
Circle, 30m dia.30m F/1 primary, 2m adaptive secondary
GEMINI
Key Point-Design Features
Paraboloidal primary– Advantage: Good image quality over 20 arcmin
field with only 2 reflections• Seeing-limited observations in visible• Mid-IR
– Disadvantage: Higher segment fabrication cost
Key Point-Design Features
F/1 primary mirror– Advantages:
• Reduces size of enclosure• Reduces flexure of optical support structure• Reduces counterweights required
– Disadvantages:• Increased sensitivity to misalignment• Increased asphericity of segments
Key Point-Design Features
Radio telescope structure– Advantages:
• Cass focus can be located just behind M1• Allows small secondary mirror – can be adaptive• Allows MCAO system ahead of Nasmyth focus
– Disadvantage: • Requires counterweight• Sweeps out larger volume in enclosure
0.001 0.01 0.1 1 10100
Ze
rnik
e m
od
e s
Bandwidth [Hz]
~100
~50
~20
~10
2
Controls Approach:Offloading Decentralized Controllers
aO (M1)
AO (M2)
Main Axes
LGS MCAO
Secondary rigid body
temporal avg
spatial & temporal avg
spatial & temporal avg
spatial & temporal avg
spatial avg
spatial avg
GSMT Control ConceptLGSs provide full sky coverage
Deformable M2 : First stage MCAO, wide field seeing improvement and M1 shape control
10-20’ field at 0.2-0.3” seeing
1-2’ field fed to the MCAO module
M2: rather slow, large stroke DM to compensate ground layer and telescope figure,
or to use as single DM at >3 m. (~8000 actuators)
Dedicated, small field (1-2’) MCAO system (~4-6DMs).
Focal plane
Active M1 (0.1 ~ 1Hz)619 segments on 91 rafts
Enabling Techniques
Active and Adaptive Optics– Active Optics already integrated into Keck, VLT,
Gemini, Subaru, Magellan, …– Adaptive Optics “added” to CFHT, Keck, Gemini,
VLT, …
Active and Adaptive Optics will have to be integrated into GSMT Telescope and Instrument concepts from the start
Enclosures
Design options under study
Response to Wind
Current concept will now go through “second iteration” of design in response to wind analysis
Fig. 4-7 – Central Raft Displacement Power Spectral DensityVent Gates Open, Wind Screen Open, Pointing into Wind, Zenith Angle = 30 deg.
0.001
0.01
0.1
1
10
100
0.1 1 10 100
Frequency (Hz)
PS
D (
m/s
qrt
(Hz)
)
TX
TY
TZ
Goal: 8000 actuators30cm spacing on M1
Options: low- to high-order • Compensate for wind-driven M1 distortions• Deliver high Strehl, mid-IR images with low emissivity• Deliver high-Strehl, near-IR images
Adaptive M2 Intrinsic to Point Design
Key Point-Design Features
2m diameter adaptive secondary mirror– Advantages:
• Correction of low-order M1 modes• Enhanced native seeing• Good performance in mid-IR• First stage in high-order AO system
– Disadvantages:• Increased difficulty (i.e., cost)
Sky Coverage vs Wavelength; Strehl for an Adaptive M2 (single laser guide star; Rigaut, 2001)
GSMT Implementation Concept- MCAO/AO foci and instruments
MCAO opticsmoves with telescope
Narrow field AO ornarrow field seeing limited port
MCAO Imagerat vertical Nasmyth
elevation axis
4m
Oschmann et al (2001)
MCAO Near-IR Imager (1:1 Unfolded)
40 mm Pupil
~2 arc minute field
Instruments• Telescope, AO and instruments must be
developed as an integrated system
• NIO team developing design concepts– Prime focus wide-field MOS
– MCAO-fed near-IR MOS
– MCAO-fed near-IR imager
– AO-fed mid-IR HRS
– Wide-field deployable IFU spectrograph
• Build on extant concepts where possible
• Define major design challenges
• Identify needed technologies
Optical “seeing improvement” using low order AO correction
16 consecutive nights of adaptive optics the CFHT
Image profilesare Lorenzian
Multi-Object Multi-Fiber Optical Spectrograph (MOMFOS)
•20 arc-minute field
• 60-meter fiber cable• 800 0.7” fibers
• 4 spectrographs, 200 fibers each• VPH gratings• Articulated collimator for different resolution regimes
Resolution Example ranges with single grating• R= 1,000 350nm – 650nm• R= 5,000 470nm – 530nm• R= 20,000 491nm – 508nm
• Detects 13% - 23% of photons hitting the 30m primary
Prime Focus MOMFOS
Barden et al (2001)
Key Point-Design Features
MOMFOS located at prime focus– Advantages
• Fast focal ratio leads to reasonably-sized instrument• Adaptive prime focus corrector allows enhanced seeing
performance
– Disadvantages• Issues of interchange with M2
MOMFOS with Prime Focus Corrector
Conceptual design fits in a 3m dia by 5m long cylinder
R=20000mode
R=5000mode
R=1000mode
MOMFOS Spectrograph
500mm pupil; all spherical optics
Spot Diagrams for Spectrograph
R=1000 case with 540 l/mm grating.
R=5000 case with 2250 l/mm grating.
350 nm 440 nm 500 nm 560 nm 650 nm
470 nm 485 nm 500 nm 515 nm 530 nm
On-axis
On-axis
Circle is 85 microns equal tosize of imaged fiber.
Barden et al (2001)
Key NIO Activities in 2001
• Core NIO team in place and working• Science case studies underway• Point design structural concept developed by SGH• Wind loading test data analyzed • AO system concept being developed• Instrument concepts
• MCAO imager• MCAO NIR MOS• IFU spectrograph• Wide-field prime-focus MOS• High resolution mid-IR spectrograph
• Chilean site characteristics assembled• Initial analysis of point design underway
Objectives: Next 2 years Develop point design for GSMT & instruments Develop key technical solutions
– Adaptive optics– Active compensation of wind buffeting– Mirror segment fabrication
Investigate design-to-cost considerations Involve the community in defining GSMT science and
engineering requirements Involve the community in defining instrumentation
options; technology paths Carry out conceptual design activities that support and
complement other efforts Develop a formal partnership to build GSMT
Objectives: Next Decade • Complete GSMT preliminary design (2Q 2005)• Complete final design (Q4 2007)• Serve as locus for
– community interaction with GSMT consortium– ongoing operations– defining; providing support capabilities– defining interactions with NGST
Key Milestones2Q01: Establish initial science requirements
• 3Q01: Complete initial instrument concepts
• 3Q01: Complete initial point design analysis
• 2Q02: Identify key technology studies
• 1Q03: Fund technology studies
• 1Q03: Complete concept trade studies
• 2Q03: Develop MOUs with partner(s)
• 2Q03: Initiate Preliminary Design
• 4Q03: Complete SRM; establish science requirements
• 2Q05: Complete Preliminary Design
• 4Q05: Complete next stage proposal
Resources: 2001-2002
• NIO activities: $3.6M – Support core NIO staff (‘skunk works team’)
• Analyze point design• Develop instrument and subsystem concepts
– Support Gemini and NOAO staff to• Explore science and instrument requirements • Develop systems engineering framework
– Support community studies:• Enable community efforts: science; instruments• Enable key external engineering studies• Support alternative concept studies
Resources: Next Decade
• $15M in CY 2003-2006 from NOAO base
– Enables start of Preliminary Design with partner
• $25M in CY 2007-2011 from NOAO base
• Create a ‘wedge’ of ~$10M/yr by 2010
– Enables NOAO funding of
• Major subsystem
• Instruments
• Operations