toward the ao for the european elt
DESCRIPTION
Toward the AO for the European ELT. Norbert Hubin European Southern Observatory. http://www.eso.org/sci/facilities/develop/ao.html. Outlines. E-ELT Project: Telescope & instrument/AO roadmap Pathfinders supporting the ELTs Adaptive telescope progresses - PowerPoint PPT PresentationTRANSCRIPT
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Toward the AO for the European ELT
Norbert HubinEuropean Southern Observatory
http://www.eso.org/sci/facilities/develop/ao.html
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E-ELT Project: Telescope & instrument/AO roadmap
Pathfinders supporting the ELTs
Adaptive telescope progresses
Single & Multi-Conjugate AO for MICADO
Single conjugate & Laser tomography for HARMONI
Single conjugate & Laser tomography for METIS
Conclusions
Outlines
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• 40-m class telescope optical-infrared telescope
• Segmented primary mirror • Adaptive Optics assisted telescope
• Multi-LGSs side launched • Diffraction limited performance: 12mas@K-band Wide field of view: 10 arcmin
• Mid-latitude site (Amazones/Chile)• Fast instrument changes• VLT level of operations efficiency.
The E-ELT ProjectThe Telescope
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The E-ELT ProjectAdaptive telescope
4
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Adaptive 2.5 m M4 unit for 39 m
4974 contactless actuators in optical area
Max 160 µm stroke
31.5 mm pitch, triangular pattern
2480/2387 mm diameter
Segmented Zerodur 1.95mm thin shell (6 petals)
Backplate in Zerodur/SiC TBC
Removable Actuator Brick design (198 bricks)On board M4 electronics
Remote M4 Control System
Flex joint hexapods for M4 Positioning System
Large bearing + cable wrap for Nasmyth selector
Mass: 10 tons
Power: 8.4 kW
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Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
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Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• 1st Light Instruments
SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO
MOAO: Multi-Object AO XAO: Extreme-AO
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Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• 2nd Pool Instruments
SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO
MOAO: Multi-Object AO XAO: Extreme-AO
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Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• XAO Instrument
SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO
MOAO: Multi-Object AO XAO: Extreme-AO
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Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• Various AO Flavors
SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO
MOAO: Multi-Object AO XAO: Extreme-AO
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All AO systems for E-ELT are challenging & costly: Many new concepts are still in demonstration phase or have not been fully
operated on smaller telescopes for science Pathfinders Technologies required are often one step behind Dev. needed Operation, Control & calibration strategies are still being figured out
crucial effective operation of AO system for science Pathfinders
Global vision is essential to reduce cost & risks for all 1 observatory cannot cope with all challenges alone Fair collaboration is
highly desirable: TMT-GMT-ESO-LBT-Gemini-Keck-WHT-SUBARU... Reasonable global pathfinding vision, good view of essential technological
bricks & cross fertilization of ideas between teams is vital• Adaptive telescope: MMT- LBT- Magellan -VLT- E-ELT…• MCAO: MAD- Solar MCAO- Gems• GLAO-LTAO: MMT, SAM, MAD, AOF, CANARY• MOAO: Village, CANARY, RAVEN EAGLE• XAO- High contrast: Gemini, VLT, SUBARU, LBT? EPICS• Lasers, DMs, RTC, WFS detectors, smart algorithms, vibration control, operation…
Global vision & walking before running
Philoso
phical s
lide
SORRY
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AOF pathfinder
27/05/2013AO4ELT - Firenze 12
Single project structure covering all phases Now in Testing
GRAAL GALACSI DSM ASSIST
4LGSF
Important R&D component embedded in AOF Project
UT4 Upgrade
NGC SPARTA (
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ESO AOF: Pathfinding Role for EELT
“Soft” benefits: Hands-on experience with an adaptive telescope New AO modes: GLAO, LTAO & of course SCAO Tight error budgets, high Strehl (GALACSI NFM,
ERIS) Calibration strategy, including on-sky, synthetic Real Time Computer: AOF SPARTA brought us
high up on learning curve How to operate an adaptive telescope efficiently
Concrete Benefits: EELT M4 is directly inspired from the DSM SAGEM benefits from the synergy of thin shells (DSM, proto M4, M4 monolithic) The Laser developed and funded by AOF is “as is” usable by EELT The Launch telescope developed by AOF is “as is” usable by EELT ESO has delivered a < 1e- RON detector @ 1.35 kHz !!! (with help from
community: Ocam, FirstLight)
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Validate control strategy: AOF as 1st step
AOF control/operation strategy good starting point for end-to-end control strategy of ELT
SCAO GLAO LTAO
ELT more complex though Segmented M1 5 mirror design to control Less rigid structure LGS operation more complex Telescope metrology overlaps with AO metrologies MCAO with one DM in telescope
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Validate end-to-end acquisition sequence (i.e AOF)
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TELESCOPE AO DESIGN & TECHNOLOGY DEVELOPMENT
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Adaptive 2.5 m M4 unit for 39 m4974 contactless actuators in optical area
Max 160 µm stroke
31.5 mm pitch, triangular pattern
2480/2387 mm diameter
Segmented Zerodur 1.95mm thin shell (6 petals)
Backplate in Zerodur/SiC TBC
Removable Actuator Brick design (198 bricks)
On board M4 electronics
Remote M4 Control System
Flex joint hexapods for M4 Positioning System
Large bearing + cable wrap for Nasmyth selector
Mass: 10 tons
Power: 8.4 kW
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Mirror technology optimization: Development of new concepts for more reliable co-located
sensors (more reliable electrical interface, easier installation) applicable to both glass and SiC M4 Unit solutions
New design of Brick interfaces to fulfill SiC manufacturing uncertainties
Demonstration prototype design on-going Next steps: Demonstration prototype development &
Completion of the Preliminary Design
M4 Unit Preliminary Design Contract
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New Actuator bricks design
The actual design of the brick is the one that will be tested on the updated demonstration prototype
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M4 Demonstration Prototype (DP) design
The DP is representative of most critical aspects of the M4U: bricks, Reference body design, shell, actuator pattern, cophasing, actuator/capsens, cooling plant, local control system.222 actuators 453.2 x 796 x 300mm
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Error budget estimate for M4 unit only
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2.5 m M5 Tip-tilt Unit prototype LCS
Purpose • Verify architecture principles and ICD towards the contractors, provide worked example as reference to construction contract. • Verify our requirements and development standards • Amend requirements and development standards, if necessary • Provide environment to verify active damping strategies
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Instruments & Modules
23
CAM MCAO
IFU LTAO(GLAO)
SCAO
SCAO
MIR SCAOLTAO – not in cons. phase
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From Single to Multi-Conjugate AO for MICADO
SCAO: Proposed as part of MICADO, a complementary AO capability for initial highest performance on compact targets. Also considered as risk mitigation & diffraction limited science before MAORY arrives (TBC)
Wavefront sensor (type depending on performance & dynamic range)
M4 adaptive mirror corrector (baseline fitting error 142 nm rms) ~50cm sampling on M1
Additional telescope error budget to be taken into account.
MCAO: MAORY good, uniform performance over full field with high sky coverage. MAORY also proposes to include a SCAO mode for on-axis peak-Strehl performance.
SCAO Sr(K) = 76% SCAO Sr(K) = 69%
No telescope WFE With telescope WFE (very preliminary 42 m)
Courtesy: Le Louarn-ONERA
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MAORY Strehl performance (0.8” seeing)
Sky coverage Galactic Pole No telescope error budget included yet
6 LGSs side launched 3 NGSs (IR WFSs) 0.6 µm < < 2.4 µm S.R. >50% in K over 2’ Central 1’ clear DM conjugated at 4km, 12.7km Two output ports
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MAORY ensquared energy performance
Performance to be updated for 39 m telescope Telescope error budget to be added
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Managerial: Phase A study Nov 2007 – Dec 2009 MCAO module approved by ESO as part of first-light instrumentation to serve E-ELT
diffraction-limited camera MICADO; however awaiting from E-ELT funding Project plan for next phases under consolidation Negotiations between ESO and INAF (lead institute) are well advanced INAF is supporting the project through its Directorate of Science Current Consortium organization: INAF; Durham Univ; Obs. de Paris/LESIA; ESO
MAORY for MICADO on-going work
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Consolidation of 20 W Raman fiber laser developed by ESO/TOPTICA
MAORY optical design trade-offs: alternative DM sizes, ADC, dichroic, LGS WFSs…
Sodium density profile measurements on-axis and in FoV (UBC collaboration
E2V Manufacturing of WFS detector: CMOS 840^2 pixels with 4eRON, 700Hz
Test controller development for the detector above: LAM & ESO GMT?
Smart algorithms for MCAO… reconstruction in collaboration with Linz team
MAORY related on-going work I
1377 act. Piezo DM for SPHERE
with its drive electronics
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Laser spot truncation in SH WfSing see Poster Miska et al.
IR 320x256 eAPD array required for low WFSing in MAORY, LTAO,
SCAO?
Medium size piezo-DM: addressing the recent DM manufacturing
obsolescence problem in collaboration with TMT & CILAS
Alternative DM solutions: XINETICS, MZA, MG-ADS
Global collaborative effort to establish a RTC development plan & strategy
for E-ELT AO instruments (U. Durham, LESIA, TNO, MPIA?, ESO) goal
coordinate RTC efforts with all E-ELT Consortia
MAORY related on-going work II
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Sodium spot elongation truncation using full tomography information
Triangle: Non Gaussian, 2x2 NGS, Diamond: 6x6 NGS Frim3D reconstr.Impact on LO or truth WFS, but truncation is ok fine on gaussian and non gaussian sodium profiles
SEE MISKA et al. poster on that topic
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WFS detectors & controllers
31
NIR SELEX detector GRAVITY320x256 eAPD array
RON<3e @ 1k frames/s; 47KelvinLow order WFS for MAORY-LTAO
But also RAPID @ LETI
E2V840x840 pixels; 24-μ pixels RON 3e @ 700 Hz frame/s delivery Q4/2013-Q1/2014
E2V + LAM Potential detector for SCAO?240x240 pixels RON 0.2e @ 1.5kHz
1.6k x1.6k?
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32
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Deformable mirror & RTC path finders
RTC box
Co-processing cluster
LGS tomography with 4 LGS WFSs 40x40 @ 1 kHz
CILAS 1370 actuators piezo DM with4.5 mm pitch
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Single conjugate & Laser Tomography AO for HARMONI
SCAO: Proposed as part of HARMONI, a complementary AO capability for highest performance on “bright” targets: Solar system, High contrast science, GC…
Wavefront sensor (optimized for high contrast, differential tracking capability, …)
wavefront sensor: Visible or IR or both?
M4 adaptive mirror corrector (baseline fitting error 142 nm rms) ~50cm sampling on M1
GLAO: Enhanced seeing capability using NGS wavefront sensors?: Earliest galaxies?
LTAO: High throughput, low emissivity, high sky coverage, “High” Sr performance required for faint targets: QSOs, GRBs, High-z G, etc…
6 Laser Guide stars side launched 2’ diameter2 IR Natural Guide Star corrected with μDMUses M4 adaptive mirror (baseline fitting error 142 nm rms) High throughput & low emissivity
LGS
NGS
4.2’
120”
60”
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Trade-offs on number / position of LGSs
LTAO: 6LGS, 4 laser launch stations (LLS), TT stars close to center of FOV500Hz, 500 iterations, 2 frames delaySeeing 0.8’’, L0=25m, tau0~3msImportance of Cn2 profile assumptions for performance estimates M. Sarazin et al.9 layers simulated, 9 layers reconstructed (unless otherwise noted)
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Single conjugate and Laser Tomography AO for HARMONI
Without telescope WFE With telescope WFE
Sr(K) =54% Sr(K) = 48.5 %
Semi-analytic simulations for 39m telescope, LGSs @ 1’ (radius), 6LGSs40 atmospheric layers simulated, 7 reconstructedPSF available for different wavelengths under request: 0.8, 1.0, 1.2, 1.6, 2.2, 10.0 um
On-axis PSFWith and without telescope WFE (very preliminary error budget)Seeing=0.67 @ 30 degrees
Contain some “reasonable” TT jitter (±3mas rms); pessimistic (TBC)? telescope wind-skake & optimum control of low order modes critical
Courtesy: Le Louarn-ONERA
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LTAO performance (from Phase A 42 m)
NOMINAL CONDITION; Sseeing = 0.8; Zenith = 0°; θ0 = 2.08"
lambda (nm) 900 1250 1650 2200 3500 4800 10500
Ensquared Energy (%)
Width 10 mas 10,3 21,1 26,1 26,4 17,8 13,7 3,9
Width 20 mas 15,1 32,1 42,5 48,5 45,6 37 14,3
Width 40 mas 18,2 37,8 53,6 63,8 62,8 61 35,1
Width 60 mas 22,4 40,5 56,3 67,8 75,9 69,1 54,2
Width 80 mas 23,2 42,4 58,2 70,2 79,8 80,1 63,8
Width 100 mas 25,6 44,8 59,5 71,7 81,3 84,6 67,5
Strehl Ratio (%) 5,5 18,8 35,3 52,7 75,6 90,5 96,9
FWHM (seeing limited) [mas] 646 609 586 546 483 442 357
FWHM (ATLAS) [mas] 8,2 9 10,1 12,1 17,6 23,7 49,1
FWHM (Diffraction) [mas] 4,4 6,1 8,1 10,8 17,2 23,6 49,6
HARMONI / SIMPLE
METIS
OPTIMOS / EAGLE like
ATLAS sky coverage
Perf SC (pole)
52 % SR in K 92 %
40 % SR in K 96%
35 % SR in K 97%
13 % SR in K
100 %
Without telescope error budget to be updated for 39 m
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Impact of telescope design change (4239m) Design optomechnical implementation of telescope metrology,
LTAO WFSing, and instrument pre-optics to ensure optimum configuration
Ensure good maintenance access on whole Nasmyth platform Progress on end-to-end Wavefront control strategy to ensure
completeness of metrology & AO sensor requirements Major work on-going!
Instrumentation arrangement optimization on E-ELT Nasmyth platform
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On-going work for LTAO implementation at Nasmyth I
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Option 3 – Gravity invariant cryostatBig optics, but all static
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From SCAO to LTAO for METIS
SCAO Excellent on-axisIntegrated in METIS
Minimize residual jitter
‘simple’ first light AO
LTAOWide(r) field performanceAccepts fainter GS(s)
Increased sky coverage
LGS configuration trade-off on-going
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SCAO for METIS
SCAO internal to METIS Cold, low (M)IR background
Dichroic first optic inside METIS Cold! Splits at ~2.5 micron Full METIS field ~18x18”
Large field selector Full METIS field Allows or field de-rotation
~40x40 sub-apertures IR WFS
Embedded sources Selex experience Gravity
Pyramid WFS Detector available But extended sources?
ELT Focus
METIS Entrance Window
Dichroic
Field Selector
Pupil de-rotator
ADC?
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LTAO Simulations27 May 20132.2 µm 3.7 µm 10 µm
AO Only
AO + Telescope OnlyESO Octopus Simulations/Miska Le Louarn
Best case scenario
LTAO Simulations
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Preliminary design of M4 unit Consolidation of MAORY Project plan for next phases Pursue technology development for MAORY Optical design trade-off incl. 39 m update Update Nasmyth platform configuration: telescope metrology-
LTAO – HARMONI & METIS Update performance estimates/error budgets for the different
AO capabilities Consolidate interfaces with instruments
Next steps
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Conclusions
An aggressive AO program is being developed for the VLT AO pathfinders for E-ELT are on-going @ VLT, WHT,… Major efforts & collaborations to bring key technologies to
appropriate TRL Facilitating AO community effort to address remaining key AO
fundamental issues (calibration, identification, control, tomography, LGS & NGS WFSing, simulation….)
Preparing for construction of E-ELT AO capabilities Setting up Consortium for the AO instrumentation The main power of the E-ELT will reside in achieving, with the
help of AO, a spatial resolution never achieved at optical/infrared wavelength to this depth before.
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THANK YOU for your attention