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1 CANARY Laser Guide Star Multi-Object Adaptive Optics (LGS MOAO) E-ELT PATHFINDER ON-SKY DEMONSTRATOR FOR EAGLE Richard Myers Durham University Royal.

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Presentation on theme: "1 CANARY Laser Guide Star Multi-Object Adaptive Optics (LGS MOAO) E-ELT PATHFINDER ON-SKY DEMONSTRATOR FOR EAGLE Richard Myers Durham University Royal."— Presentation transcript:

1 1 CANARY Laser Guide Star Multi-Object Adaptive Optics (LGS MOAO) E-ELT PATHFINDER ON-SKY DEMONSTRATOR FOR EAGLE Richard Myers Durham University Royal Astronomical Society

2 9 May RAS Overview CANARY Collaboration CANARY Collaboration LGS MOAO LGS MOAO General General EAGLE EAGLE Technical challenges Technical challenges Principles of CANARY demonstrator Principles of CANARY demonstrator Rayleigh LGS Rayleigh LGS Role of WHT Role of WHT Demonstration stages and timescales Demonstration stages and timescales Risk mitigation Risk mitigation Current status Current status Funding status Funding status Why “CANARY”? Falcon: 8m MOAO (study) EAGLE: 42m MOAO CANARY: MOAO demo on 4.2m WHT on La Palma, Canary Islands

3 9 May RAS CANARY Consortium Overlaps with EAGLE AO design team and SESAME team Observatoire de Paris LESIADurham UniversityIsaac Newton Group Laboratoire d’Astrophysique de Marseille UK Astronomy Technology Centre Fanny Chemla, Eric Gendron, Zoltàn Hubert, Aglaé Kellerer, Michel Marteaud, Gérard Rousset, Fabrice Vidal, Ali Basden, Sofia Dimoudi, Nigel Dipper, Colin Dunlop, Deli Geng, Andres Gueselaga, Dani Guzman, Mark Harrison, Tim Morris, Richard Myers, James Osborn, Chris Saunter, Gordon Talbot, Laura Young, Eddy Younger, Don Carlos Abrahams, René Rutten, Thierry Fusco, David Henry, Andy Longmore, Brice Leroux ONERA

4 9 May RAS Laser Guide Star Multi-Object Adaptive Optics (LGS MOAO) LGS MOAO Schematic [Courtesy ESO]

5 9 May RAS EAGLE MOAO requirements and baseline implementation NIR Multi-Integral Field Unit (IFU) for 42m E-ELT NIR Multi-Integral Field Unit (IFU) for 42m E-ELT Wide IFU patrol field ≥ 5 arcmin with ≥ 20 such IFUs Wide IFU patrol field ≥ 5 arcmin with ≥ 20 such IFUs ≥ 30% energy in arcsec spatial element in H-band ≥ 30% energy in arcsec spatial element in H-band Multiple LGS (≥ 6), multiple NGS (≥ 3) Multiple LGS (≥ 6), multiple NGS (≥ 3) Closed loop control of M4 telescope adaptive mirror Closed loop control of M4 telescope adaptive mirror Open loop control of high order (≥ 100x100 actuator) Deformable Mirror (DM) in each IFU channel Open loop control of high order (≥ 100x100 actuator) Deformable Mirror (DM) in each IFU channel

6 9 May RAS Technical challenge and proposed mitigation Open loop control of high order DMs Open loop control of high order DMs calibration calibration ELT LGS ELT LGS Spot elongation Spot elongation High accuracy wide field tomography High accuracy wide field tomography Real-time control (RTC) Real-time control (RTC) Algorithms Algorithms Scale of implementation Scale of implementation Laboratory Demonstration: SESAME: working now Staged On-sky Demonstration of SINGLE channel: CANARY: Goals: * demonstrate MOAO in EAGLE configuration, * verify design models, * develop techniques, e.g., calibration, RTC

7 9 May RAS LGS Wavefront Sensor (WFS) Spot Elongation due to sodium layer depth (central LGS) Cone Effect LGS WORSE for ELTs turbulence

8 9 May RAS CANARY LGS MOAO demo method Key technology: RAYLEIGH LGS (RLGS) (e.g., SOR, WHT, MMT, SOAR, LBT LGS study) These use pulsed lasers with temporal WFS range gating These use pulsed lasers with temporal WFS range gating to select LGS height and extension (range gate depth) to select LGS height and extension (range gate depth) The Rayleigh LGS Altitude and extension are programmable The Rayleigh LGS Altitude and extension are programmable They can emulate the spot elongation & cone-effect geometry of a SODIUM LGS on a MUCH LARGER telescope They can emulate the spot elongation & cone-effect geometry of a SODIUM LGS on a MUCH LARGER telescope SO: SO: 85 km sodium LGS → 8.5km Rayleigh LGS 85 km sodium LGS → 8.5km Rayleigh LGS 10km sodium layer → 1km range gate depth 10km sodium layer → 1km range gate depth 42m E-ELT → 4.2m WHT 42m E-ELT → 4.2m WHT In principle: can emulate sodium density evolution too In principle: can emulate sodium density evolution too

9 9 May RAS However… BUT: BUT: This scaling is not perfect This scaling is not perfect Atmosphere and wavelength are not scaled Atmosphere and wavelength are not scaled There will be additional uncorrected turbulence in demo compared to ELT There will be additional uncorrected turbulence in demo compared to ELT Need to reduce LGS separation to emulate ELT meta- pupil overlap at a given altitude Need to reduce LGS separation to emulate ELT meta- pupil overlap at a given altitude SO NEED: SO NEED: Concurrent Natural Guide Star (NGS) tomography Concurrent Natural Guide Star (NGS) tomography Record corrected wavefront (truth sensor) as well as the near-IR image (Point Spread Function) Record corrected wavefront (truth sensor) as well as the near-IR image (Point Spread Function) To check that current MOAO correction is as predicted for current atmosphere To check that current MOAO correction is as predicted for current atmosphere

10 9 May RAS William Herschel Telescope 4.2m Alt-Az, La Palma 4.2m Alt-Az, La Palma Operational Rayleigh LGS: GLAS Operational Rayleigh LGS: GLAS Grond-laag Laser Adaptieve optiek Systeem (Ground-layer Laser AO System) 18 W 515nm 18 W 515nm Launch System Launch System 35cm telescope above M2 35cm telescope above M2 Safety Infrastructure Safety Infrastructure No fly zone No fly zone Launch permission Launch permission Traffic Control Traffic Control MK clone MK clone MASS/DIMM 20m from WHT MASS/DIMM 20m from WHT SCIDAR 340m from WHT SCIDAR 340m from WHT

11 9 May RAS GLAS WHT LGS Facility ING - Astron - Durham Variation of closed-loop (●) and open-loop (○) Gaussian fit FWHM versus angular distance from centre of field for a 20s J-band image. Turbulence profile approx 50% at ground, 15% at 4km, and 35% at 16km. LGS altitude of 15km. NAOMI AO System: UKATC-Durham-ING INGRiD imager: ING OASIS IFU: Lyon

12 9 May RAS GLAS Software Description

13 9 May RAS WHT Nasmyth (GHRIL) Large, undedicated Nasmyth enclosure for guest instruments Large, undedicated Nasmyth enclosure for guest instruments 2.5 × 1.34 m opt bench 2.5 × 1.34 m opt bench Services Services

14 9 May RAS GHRIL NASMYTH

15 9 May RAS CANARY Demo Stages Phase A 2010 Phase A × Natural Guide Stars (in 3’ field) open loop control of low order (8 × 8 actuator) Deformable Mirror (DM) 3 × Natural Guide Stars (in 3’ field) open loop control of low order (8 × 8 actuator) Deformable Mirror (DM) Natural Guide Star Truth Wavefront Sensor, Near-IR imager Natural Guide Star Truth Wavefront Sensor, Near-IR imager Phase B 2011 Phase B 2011 Add 4 × LGS open loop control of low order DM Add 4 × LGS open loop control of low order DM Concurrent NGS tomography maintained Concurrent NGS tomography maintained Phase C 2012 Phase C 2012 Closed loop LGS/NGS control of low-order DM Closed loop LGS/NGS control of low-order DM Open loop control of high-order DM (up to 32 × 32 actuator) Open loop control of high-order DM (up to 32 × 32 actuator) Full-up EAGLE demo Full-up EAGLE demo

16 9 May RAS Phase A : NGS MOAO Components: Components: Low-order 8x8 DM Low-order 8x8 DM 3 x EMCCD open-loop NGS WFSs 3 x EMCCD open-loop NGS WFSs Open-loop optimised Fast Steering Mirror (SPHERE design) Open-loop optimised Fast Steering Mirror (SPHERE design) Diagnostic Systems: Diagnostic Systems: 1 x EMCCD closed-loop NGS WFS (Truth Sensor) 1 x EMCCD closed-loop NGS WFS (Truth Sensor) High speed DM figure sensor High speed DM figure sensor NIR Imaging camera (loan courtesy ESO) NIR Imaging camera (loan courtesy ESO) WHT Nasmyth Calibration Unit NGS Pickoffs 3 x NGS WFS NGS FSM Low-order DM Science Verification Truth Sensor Figure Sensor GHRIL Derotator Phase A: NGS MOAO

17 9 May RAS Phase B: Low-order LGS MOAO New modules include: New modules include: Electronically shuttered LGS WFS CCD (Lincoln Lab) Electronically shuttered LGS WFS CCD (Lincoln Lab) Modified GLAS launch, LGS dichroic and relay system Modified GLAS launch, LGS dichroic and relay system WHT Nasmyth Calibration Unit NGS Pickoffs 3 x NGS WFS NGS FSM Low-order DM Science Verification Truth Sensor LGS Pickoffs 4 x LGS WFS GHRIL Derotator Figure Sensor GLAS Laser LGS Rotator GLAS BLT Diffractive Optic LGS FSM LGS Dichroic Phase B: Low-order LGS MOAO

18 9 May RAS Phase C: High-order LGS MOAO Closest resemblance to proposed EAGLE MOAO implementation Closest resemblance to proposed EAGLE MOAO implementation Closed-loop low-order DM conjugated to ground layer Closed-loop low-order DM conjugated to ground layer Open-loop MEMS DM Open-loop MEMS DM SPARTA (ESO VLT) type accelerated Real-Time Computer SPARTA (ESO VLT) type accelerated Real-Time Computer NOTE: LOW-ORDER LTAO CAPABILITY NOTE: LOW-ORDER LTAO CAPABILITY WHT Nasmyth Calibration Unit NGS Pickoffs 3 x NGS WFS NGS FSM Low-order DM Science Verification Truth Sensor Figure Sensor LGS Pickoffs 4 x LGS WFS GHRIL Derotator MEMS DM GLAS Laser LGS Rotator GLAS BLT Diffractive Optic LGS FSM LGS Dichroic Phase C: High-order woofer-tweeter LGS MOAO (woofer closed loop)

19 9 May RAS Key Components NGS WFS NGS WFS E2V EMCCDs (asterisms with 4 NGS in 3’ needed) E2V EMCCDs (asterisms with 4 NGS in 3’ needed) LGS WFS LGS WFS Lincoln Lab Gated CCDs Lincoln Lab Gated CCDs Fast Steering Mirror Fast Steering Mirror Surface Sensing SPHERE Design Surface Sensing SPHERE Design Low order DM Low order DM Adonis (ESO 3.6m) Adonis (ESO 3.6m) High order DM High order DM BMM 32 × 32 MEMS – just delivered BMM 32 × 32 MEMS – just delivered Real-time Computer Real-time Computer PC-based with Evolution to ESO SPARTA system PC-based with Evolution to ESO SPARTA system Phase A NGS Design: Paris LESIA

20 9 May RAS“De-Risking” Figure Sensor (DMC) Figure Sensor (DMC) High-speed LUPA 300 CMOS detector + FPGA (IAC collab) High-speed LUPA 300 CMOS detector + FPGA (IAC collab) Proof of concept trial currently being integrated in Durham Proof of concept trial currently being integrated in Durham RTC RTC First version based on working PC-based system First version based on working PC-based system Contract with ONERA/Shaktiware Contract with ONERA/Shaktiware On-site component tests October 2008 On-site component tests October 2008 LGS asterism test: Diffractive Optical Element (Herriot-Watt) LGS asterism test: Diffractive Optical Element (Herriot-Watt) Gated CCD test on-sky Gated CCD test on-sky Test Figure Sensor in WHT environment Test Figure Sensor in WHT environment

21 9 May RAS Current Status NGS main path opto- mechanical concept complete NGS main path opto- mechanical concept complete Alignment/calibration procedures Alignment/calibration procedures LGS pickoff and relay optical design complete LGS pickoff and relay optical design complete 2 simulations running 2 simulations running using YAO run by A. Kellerer using YAO run by A. Kellerer Using Durham AO simulation platform (DASP) by A. Basden Using Durham AO simulation platform (DASP) by A. Basden Next: Next: Comparative simulation using EAGLE design codes Comparative simulation using EAGLE design codes ONERA/Durham ONERA/Durham Design Reviews June 2008 Design Reviews June 2008 Phase A PDR, B/C CoDR Phase A PDR, B/C CoDR RTC first contract June 2008 RTC first contract June 2008 Phase A Space Envelope At WHT Nasmyth Phase B Optics

22 9 May RAS PHASE B

23 9 May RAS Phase C

24 9 May RAS

25 9 May RAS

26 9 May RAS Funding Status UK (STFC) UK (STFC) France (various) France (various) EU FP7 Preparatory Fund EU FP7 Preparatory Fund EU OPTICON JRA-1 – applied EU OPTICON JRA-1 – applied ESO-led ESO-led Includes additional WHT nights Includes additional WHT nights Further STFC support for final phase - applied Further STFC support for final phase - applied Further French funding proposals - to be made Further French funding proposals - to be made Funded, enough for first two phases


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