1. Toward the AO for the European ELT Norbert Hubin European Southern Observatory http://www.eso.org/sci/facilities/develop/ao.html

2. n E-ELT Project: Telescope & instrument/AO roadmap n Pathfinders supporting the ELTs n Adaptive telescope progresses n Single & Multi-Conjugate AO for MICADO n Single conjugate & Laser tomography for HARMONI n Single conjugate & Laser tomography for METIS n Conclusions Outlines

3. 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 Project The Telescope

4. The E-ELT Project Adaptive telescope 4

5. 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

6. Instruments - First Light AOModeλ (µm)ResolutionFoV / SamplingAdd. Mode E-CAM – 2023 SCAO, MCAO - IMG - MRS 0.8 – 2.4BB, NB 3000 53.0” / 3 masAstrometry 40mas Coronography E-IFU – 2023 SCAO, LTAO - IFU0.5 – 2.44000 10 000 20 000 0.5×1.0” / 4mas 5.0×10.0” / 40mas Coronography E-MIDIR – 2024/2028 SCAO, LTAO - IMG - MRS - IFU 3 – 13 3 - 13 3 - 5 BB, NB 5000 100 000 18” / 12 mas 0.4”×1.5” / 4 mas Coronography Polarimetry E-HIRES - 2024/2028 SCAO - HRS 0.37 – 0.71 0.84 – 2.50 200 000 120 000 0.82” 0.027”×0.5” Polarimetry E-MOS - 2024/2028 MOAO Slits IFUs 0.37 – 1.4 0.8 – 2.45 300- 2500 5000 – 30 000 4000 – 10 000 6.8” / 0.1” 420’ / 0.3” 2” / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS - 2027/2030 XAOEPOL IFS 0.6 – 0.9 0.95 – 1.65125 – 20 000 2.0” / 2.3 mas 0.8“ / 1.5 mas Coronography Polarimetry Instrument Roadmap The E-ELT Project

7. Instruments - First Light AOModeλ (µm)ResolutionFoV / SamplingAdd. Mode E-CAM – 2023 SCAO, MCAO - IMG - MRS 0.8 – 2.4BB, NB 3000 53.0” / 3 masAstrometry 40mas Coronography E-IFU – 2023 SCAO, LTAO - IFU0.5 – 2.44000 10 000 20 000 0.5×1.0” / 4mas 5.0×10.0” / 40mas Coronography E-MIDIR – 2024/2028 SCAO, LTAO - IMG - MRS - IFU 3 – 13 3 - 13 3 - 5 BB, NB 5000 100 000 18” / 12 mas 0.4”×1.5” / 4 mas Coronography Polarimetry E-HIRES - 2024/2028 SCAO - HRS 0.37 – 0.71 0.84 – 2.50 200 000 120 000 0.82” 0.027”×0.5” Polarimetry E-MOS - 2024/2028 MOAO Slits IFUs 0.37 – 1.4 0.8 – 2.45 300- 2500 5000 – 30 000 4000 – 10 000 6.8” / 0.1” 420’ / 0.3” 2” / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS - 2027/2030 XAOEPOL IFS 0.6 – 0.9 0.95 – 1.65125 – 20 000 2.0” / 2.3 mas 0.8“ / 1.5 mas Coronography Polarimetry Instrument Roadmap The E-ELT Project 1st Light Instruments SCAO: single-conjugated AOMCAO: Multi-Conjugated-AOLTAO: Laser-Tomographic AO MOAO: Multi-Object AOXAO: Extreme-AO

8. Instruments - First Light AOModeλ (µm)ResolutionFoV / SamplingAdd. Mode E-CAM – 2023 SCAO, MCAO - IMG - MRS 0.8 – 2.4BB, NB 3000 53.0” / 3 masAstrometry 40mas Coronography E-IFU – 2023 SCAO, LTAO - IFU0.5 – 2.44000 10 000 20 000 0.5×1.0” / 4mas 5.0×10.0” / 40mas Coronography E-MIDIR – 2024/2028 SCAO, LTAO - IMG - MRS - IFU 3 – 13 3 - 13 3 - 5 BB, NB 5000 100 000 18” / 12 mas 0.4”×1.5” / 4 mas Coronography Polarimetry E-HIRES - 2024/2028 SCAO - HRS 0.37 – 0.71 0.84 – 2.50 200 000 120 000 0.82” 0.027”×0.5” Polarimetry E-MOS - 2024/2028 MOAO Slits IFUs 0.37 – 1.4 0.8 – 2.45 300- 2500 5000 – 30 000 4000 – 10 000 6.8” / 0.1” 420’ / 0.3” 2” / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS - 2027/2030 XAOEPOL IFS 0.6 – 0.9 0.95 – 1.65125 – 20 000 2.0” / 2.3 mas 0.8“ / 1.5 mas Coronography Polarimetry Instrument Roadmap The E-ELT Project 2 nd Pool Instruments SCAO: single-conjugated AOMCAO: Multi-Conjugated-AOLTAO: Laser-Tomographic AO MOAO: Multi-Object AOXAO: Extreme-AO

9. Instruments - First Light AOModeλ (µm)ResolutionFoV / SamplingAdd. Mode E-CAM – 2023 SCAO, MCAO - IMG - MRS 0.8 – 2.4BB, NB 3000 53.0” / 3 masAstrometry 40mas Coronography E-IFU – 2023 SCAO, LTAO - IFU0.5 – 2.44000 10 000 20 000 0.5×1.0” / 4mas 5.0×10.0” / 40mas Coronography E-MIDIR – 2024/2028 SCAO, LTAO - IMG - MRS - IFU 3 – 13 3 - 13 3 - 5 BB, NB 5000 100 000 18” / 12 mas 0.4”×1.5” / 4 mas Coronography Polarimetry E-HIRES - 2024/2028 SCAO - HRS 0.37 – 0.71 0.84 – 2.50 200 000 120 000 0.82” 0.027”×0.5” Polarimetry E-MOS - 2024/2028 MOAO Slits IFUs 0.37 – 1.4 0.8 – 2.45 300- 2500 5000 – 30 000 4000 – 10 000 6.8” / 0.1” 420’ / 0.3” 2” / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS - 2027/2030 XAOEPOL IFS 0.6 – 0.9 0.95 – 1.65125 – 20 000 2.0” / 2.3 mas 0.8“ / 1.5 mas Coronography Polarimetry Instrument Roadmap The E-ELT Project XAO Instrument SCAO: single-conjugated AOMCAO: Multi-Conjugated-AOLTAO: Laser-Tomographic AO MOAO: Multi-Object AOXAO: Extreme-AO

10. Instruments - First Light AOModeλ (µm)ResolutionFoV / SamplingAdd. Mode E-CAM – 2023 SCAO, MCAO - IMG - MRS 0.8 – 2.4BB, NB 3000 53.0” / 3 masAstrometry 40mas Coronography E-IFU – 2023 SCAO, LTAO - IFU0.5 – 2.44000 10 000 20 000 0.5×1.0” / 4mas 5.0×10.0” / 40mas Coronography E-MIDIR – 2024/2028 SCAO, LTAO - IMG - MRS - IFU 3 – 13 3 - 13 3 - 5 BB, NB 5000 100 000 18” / 12 mas 0.4”×1.5” / 4 mas Coronography Polarimetry E-HIRES - 2024/2028 SCAO - HRS 0.37 – 0.71 0.84 – 2.50 200 000 120 000 0.82” 0.027”×0.5” Polarimetry E-MOS - 2024/2028 MOAO Slits IFUs 0.37 – 1.4 0.8 – 2.45 300- 2500 5000 – 30 000 4000 – 10 000 6.8” / 0.1” 420’ / 0.3” 2” / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS - 2027/2030 XAOEPOL IFS 0.6 – 0.9 0.95 – 1.65125 – 20 000 2.0” / 2.3 mas 0.8“ / 1.5 mas Coronography Polarimetry Instrument Roadmap The E-ELT Project Various AO Flavors SCAO: single-conjugated AOMCAO: Multi-Conjugated-AOLTAO: Laser-Tomographic AO MOAO: Multi-Object AOXAO: Extreme-AO

11. n 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 n 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 Philosophical slide SORRY

12. AOF pathfinder 27/05/2013AO4ELT - Firenze 12  Single project structure covering all phases  Now in Testing GRAAL GALACSI DSMASSIST 4LGSF Important R&D component embedded in AOF Project UT4 Upgrade NGC SPARTA (

13. 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)

14. Validate control strategy: AOF as 1 st 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

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

16. TELESCOPE AO DESIGN & TECHNOLOGY DEVELOPMENT

17. 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

18. n Mirror technology optimization: n 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 n New design of Brick interfaces to fulfill SiC manufacturing uncertainties n Demonstration prototype design on-going n Next steps: Demonstration prototype development & Completion of the Preliminary Design M4 Unit Preliminary Design Contract

19. New Actuator bricks design The actual design of the brick is the one that will be tested on the updated demonstration prototype

20. 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

21. Error budget estimate for M4 unit only

22. 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

23. Instruments & Modules 23 CAMMCAO IFULTAO(GLAO) SCAO MIRSCAO LTAO – not in cons. phase

24. 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

25. 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

26. MAORY ensquared energy performance Performance to be updated for 39 m telescope Telescope error budget to be added

27. n 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

28. n Consolidation of 20 W Raman fiber laser developed by ESO/TOPTICA n MAORY optical design trade-offs: alternative DM sizes, ADC, dichroic, LGS WFSs… n Sodium density profile measurements on-axis and in FoV (UBC collaboration n E2V Manufacturing of WFS detector: CMOS 840^2 pixels with 4eRON, 700Hz n Test controller development for the detector above: LAM & ESO  GMT? n 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

29. n Laser spot truncation in SH WfSing  see Poster Miska et al. n IR 320x256 eAPD array required for low WFSing in MAORY, LTAO, SCAO? n Medium size piezo-DM: addressing the recent DM manufacturing obsolescence problem in collaboration with TMT & CILAS n Alternative DM solutions: XINETICS, MZA, MG-ADS n 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

30. 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

31. WFS detectors & controllers 31 NIR SELEX detector  GRAVITY 320x256 eAPD array RON<3e @ 1k frames/s; 47Kelvin Low order WFS for MAORY-LTAO But also RAPID @ LETI E2V 840x840 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?

32. 32 Pixel number “Natural Guide Star Detector” NGSD - 880x840 pixels with 840x840 sensitive pixels Detector technologyThinned backside illuminated CMOS 0.18µm Pixel Pitch24µm Pixel topology4T pinned photodiode pixel Sub-aperture20x20 pixels Array architecture42x42 sub-apertures of 20x20 pixels Pixel full well4000 e- Read noise including ADC< 3.0 e - RMS ADCs configuration20 x 880 column ADCs, 9 (goal 10) bits Frame rate700 fps up to 1000 fps with degraded performance

33. Deformable mirror & RTC path finders RTC box Co-processing cluster LGS tomography with 4 LGS WFSs 40x40 @ 1 kHz CILAS 1370 actuators piezo DM with 4.5 mm pitch

34. 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’ diameter  2 IR Natural Guide Star corrected with μDM  Uses M4 adaptive mirror (baseline fitting error 142 nm rms)  High throughput & low emissivity LGS NGS 4.2’ 120” 60”

35. Trade-offs on number / position of LGSs LTAO: 6LGS, 4 laser launch stations (LLS), TT stars close to center of FOV 500Hz, 500 iterations, 2 frames delay Seeing 0.8’’, L0=25m, tau0~3ms Importance of Cn2 profile assumptions for performance estimates  M. Sarazin et al. 9 layers simulated, 9 layers reconstructed (unless otherwise noted)

36. 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), 6LGSs  40 atmospheric layers simulated, 7 reconstructed  PSF available for different wavelengths under request: 0.8, 1.0, 1.2, 1.6, 2.2, 10.0 um  On-axis PSF  With 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

37. LTAO performance (from Phase A 42 m) NOMINAL CONDITION; Sseeing = 0.8; Zenith = 0°; θ0 = 2.08" lambda (nm) 9001250165022003500480010500 Ensquared Energy (%) Width 10 mas 10,321,126,126,417,813,73,9 Width 20 mas 15,132,142,548,545,63714,3 Width 40 mas 18,237,853,663,862,86135,1 Width 60 mas 22,440,556,367,875,969,154,2 Width 80 mas 23,242,458,270,279,880,163,8 Width 100 mas 25,644,859,571,781,384,667,5 Strehl Ratio (%) 5,518,835,352,775,690,596,9 FWHM (seeing limited) [mas] 646609586546483442357 FWHM (ATLAS) [mas] 8,2910,112,117,623,749,1 FWHM (Diffraction) [mas] 4,46,18,110,817,223,649,6 HARMONI / SIMPLE METIS OPTIMOS / EAGLE like ATLAS sky coverage PerfSC (pole) 52 % SR in K92 % 40 % SR in K96% 35 % SR in K97% 13 % SR in K100 % Without telescope error budget to be updated for 39 m

38. n Impact of telescope design change (42  39m) n Design optomechnical implementation of telescope metrology, LTAO WFSing, and instrument pre-optics to ensure optimum configuration n Ensure good maintenance access on whole Nasmyth platform n Progress on end-to-end Wavefront control strategy to ensure completeness of metrology & AO sensor requirements n Major work on-going! Instrumentation arrangement optimization on E-ELT Nasmyth platform

39. On-going work for LTAO implementation at Nasmyth I

40. Option 3 – Gravity invariant cryostat Big optics, but all static

41. From SCAO to LTAO for METIS SCAO n Excellent on-axis n Integrated in METIS  Minimize residual jitter n ‘simple’ first light AO LTAO n Wide(r) field performance n Accepts fainter GS(s)  Increased sky coverage n LGS configuration trade-off on-going

42. SCAO for METIS n SCAO internal to METIS  Cold, low (M)IR background n Dichroic first optic inside METIS  Cold!  Splits at ~2.5 micron  Full METIS field ~18x18” n Large field selector  Full METIS field  Allows or field de-rotation n ~40x40 sub-apertures n IR WFS  Embedded sources  Selex experience Gravity n Pyramid WFS  Detector available  But extended sources? ELT Focus METIS Entrance Window Dichroic Field Selector Pupil de-rotator ADC?

43. LTAO Simulations 27 May 2013 2.2 µm3.7 µm10 µm AO Only AO + Telescope Only ESO Octopus Simulations/Miska Le Louarn Best case scenario LTAO Simulations

44. n Preliminary design of M4 unit n Consolidation of MAORY Project plan for next phases n Pursue technology development for MAORY n Optical design trade-off incl. 39 m update n Update Nasmyth platform configuration: telescope metrology- LTAO – HARMONI & METIS n Update performance estimates/error budgets for the different AO capabilities n Consolidate interfaces with instruments Next steps

45. Conclusions n An aggressive AO program is being developed for the VLT n AO pathfinders for E-ELT are on-going @ VLT, WHT,… n Major efforts & collaborations to bring key technologies to appropriate TRL n Facilitating AO community effort to address remaining key AO fundamental issues (calibration, identification, control, tomography, LGS & NGS WFSing, simulation….) n Preparing for construction of E-ELT AO capabilities n Setting up Consortium for the AO instrumentation n 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.

46. THANK YOU for your attention