toward the ao for the european elt norbert hubin european southern observatory

Toward the AO for the European ELT

Norbert HubinEuropean Southern Observatory

http://www.eso.org/sci/facilities/develop/ao.html

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

• 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

The E-ELT ProjectAdaptive telescope

4

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

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


Instrument RoadmapThe E-ELT Project



E-CAM – 2023

SCAO,MCAO

- IMG- MRS

0.8 – 2.4 BB, NB3000


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


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


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



• 1st Light Instruments

SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO

MOAO: Multi-Object AO XAO: Extreme-AO



E-CAM – 2023

SCAO,MCAO

- IMG- MRS

0.8 – 2.4 BB, NB3000


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


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


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



• 2nd Pool Instruments





E-CAM – 2023

SCAO,MCAO

- IMG- MRS

0.8 – 2.4 BB, NB3000


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


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


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



• XAO Instrument





E-CAM – 2023

SCAO,MCAO

- IMG- MRS

0.8 – 2.4 BB, NB3000


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


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


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



• Various AO Flavors



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

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 (

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)

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

Validate end-to-end acquisition sequence (i.e AOF)

TELESCOPE AO DESIGN & TECHNOLOGY DEVELOPMENT

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

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

New Actuator bricks design

The actual design of the brick is the one that will be tested on the updated demonstration prototype

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

Error budget estimate for M4 unit only

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

Instruments & Modules

23

CAM MCAO

IFU LTAO(GLAO)

SCAO

SCAO

MIR SCAOLTAO – not in cons. phase

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

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

MAORY ensquared energy performance

Performance to be updated for 39 m telescope Telescope error budget to be added

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

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

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

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

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?

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

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”

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)

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

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

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

On-going work for LTAO implementation at Nasmyth I

Option 3 – Gravity invariant cryostatBig optics, but all static

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

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?

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

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

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.

THANK YOU for your attention

toward the ao for the european elt norbert hubin european southern observatory

Documents

scao hrs0

ltao img

mcao img

ltao ifu0

mas multiplex

multiobject aoxao

mrs ifu3

singleconjugated aomcao