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MultiConjugate Adaptive OpticsMultiConjugate Adaptive Opticsfrom VLTs to ELTsfrom VLTs to ELTs

J.-M. Conan(1),J.-M. Conan(1), B. Neichel(1,2), C. Petit(1), M. Nicolle(1) B. Neichel(1,2), C. Petit(1), M. Nicolle(1) T. Fusco(1), E. Gendron(2), G. Rousset (3,2,1), T. Fusco(1), E. Gendron(2), G. Rousset (3,2,1), P. Jagourel(2), F. Hammer(2)P. Jagourel(2), F. Hammer(2)

(1) ONERA – DOTA - HRA(1) ONERA – DOTA - HRA (2) Observatoire de Paris-Meudon(2) Observatoire de Paris-Meudon (3) Université Paris 7(3) Université Paris 7

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Adaptive Optics and Anisoplanatism EffectsAdaptive Optics and Anisoplanatism Effects

Isoplanatic FoV~ 20’’ Isoplanatic FoV ~ 2’’

NAOS Data ; 2,2µm ; Field of View =27’’ ; courtesy D. Rouan

Standard AO corrected FoV is very limited

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Principle of MultiConjugate AO [MCAO]MCAO allows wide FoV correction

Specificities:

multi-guide-star wavefront sensing

multi-DM correction of the turbulent volume

Expected performance:

few arcmin diffraction limited correction for NIR VLT obs. with a few GSs and a few DMs

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« Ground Layer » Adaptive Optics [GLAO]« Ground Layer » Adaptive Optics [GLAO]

GLAO: multi-GS WFS single ground DM correcting average perturbation ~ near ground turbulence

No Correction: Seeing limited

single Ground DMsingle Ground DM

GLAO: reduced apparent seeing

seeing improved and stabilizedin very large FoVgain ~2 in 10 arcmin for NIR VLT obs.

Expected performance:

FoVFoV

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MultiObject AO [MOAO] – Falcon studyMultiObject AO [MOAO] – Falcon study

Extra-galactic 3D spectrocopynear-diffraction limited correction

on tens of faint/tiny galaxies

in very large FoV

MOAO:specific correction/DM per galaxy multi-GS WFS

Expected Performance:Falcon: H band VLT obs. in 25’ FoV 60 GS for WFS

15 to 20 IFU on galaxies with 40% coupling in 250mas res. elts

see Gendron et al., C. R. Phys., 6, 2005

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OutlineOutline

• Key Features/Issues in MCAO– Multi-GS wavefront sensing

• choice of the concept (Star/Layer Oriented, MFoV…)

• Natural/Laser GS related to sky-coverage consideration

[M. Nicolle et al., JOSA A accepted ; T. Fusco et al., MNRAS accepted]

– Correction optimisation in FoV of interest ≠ GS positions

• Reconstruction of turbulent volume from WFS data (tomographic rec.)

• multi-DM control

• Current VLT MCAO/GLAO projects• MOAO for extra-galactic observations: from VLTs (8-10m) to ELTs (20 to 60m)

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Off axis pupilmetapupil

DM

On axis pupil

WFS

1 turbulent layer in altitude

1 on axis GS for WFS

1 off axis star of interest

Simplified Experimental Configuration : Off-Axis AOSimplified Experimental Configuration : Off-Axis AO

Optimal Control:Optimal Control:• reconstruction of phase in layer(s)reconstruction of phase in layer(s) iterative Kalman filteriterative Kalman filter• adequate projection onto DM(s)adequate projection onto DM(s)

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AO Bench at ONERA : BOAAO Bench at ONERA : BOA

Imaging camera (Princeton - 512)

Sources (2 stars) : fibered laser diode

Turbulent phase screen

Wave Front Sensor(Shack-Hartman 8*8) Deformable mirror

SAM (9*9)

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C. Petit et al., C. R. Physique, 6, 2005

On-Axis Star Off-Axis Star

First Experimental Demonstration of Off-Axis AOFirst Experimental Demonstration of Off-Axis AO

collaboration with L2TI-Villetaneuse-Paris 13 and ShaktiWarecollaboration with L2TI-Villetaneuse-Paris 13 and ShaktiWare

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Planned VLT Systems and Demonstrators 1/2Planned VLT Systems and Demonstrators 1/2

• 8m-VLT MAD MCAO demonstrator [ESO-Arcetri] first light end 2006

– 2’ FoV NIR imaging : 5 to 8 NGS, 2 DM (~60 act. each),

• 8m-GEMINI South MCAO [Gemini] first light 2007

– 2’ FoV NIR imaging : 5 Na-LGS + 3 TT-NGS, 3 DM (~200 act. each),

• 2x8m-LBT LINC-NIRVANA MCAO [MaxPlanck-Arcetri]

– up to 2’ FoV NIR interometric-imaging : 12 NGS, 672 act. DSM +1 or 2 DMs (~300act.)

• 8m-VLT GRAAL GLAO for HAWK-I [ESO] first light 2012

– 10’ FoV for NIR imaging : 4 Na-LGS + 1 TT-NGS, 1170 act. DSM

• 8m-VLT GALACSI GLAO for MUSE [ESO] first light 2012

– 3’’ to 2’ FoV for Vis. spectro-imaging : 4 Na-LGS + 1 TT-NGS, 1170 act. DSM

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Planned VLT Systems and Demonstrators 2/2Planned VLT Systems and Demonstrators 2/2

• Solar MCAO: – KIS (80cm-VTT, future 1.5m-GregorTel)

– NSO (70cm-DTT, future 4m-ATST)

• Laboratory demonstrators, among others: – Sesame at Obs.-Meudon – multi-GS sigle-DM configuration available

– Homer at Onera – currently in design phase, 2-DM config. planned for 2007

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MultiObject AO [MOAO] – Falcon studyMultiObject AO [MOAO] – Falcon study

Extra-galactic 3D spectrocopynear-diffraction limited correction

on tens of faint/tiny galaxies

in very large FoV

MOAO: specific correction/DM per galaxy multi-GS WFS

Expected Performance:Falcon: H band VLT obs. in 25’ FoV

60 GS for WFS 15 to 20 IFU on galaxies

with 40% coupling in 250mas res. elts

see Gendron et al., C. R. Phys., 6, 2005

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MOAO VLT versus ELT specificationsMOAO VLT versus ELT specifications

Falcon design study: 60 GS for WFS 15 to 20 IFU on galaxies with ~100 act. correction sky-coverage ~ 50% at b=30°

see Gendron et al., C. R. Phys., 6, 2005

10 m class specifications10 m class specifications• 0.5 < Z < 2 – 30.5 < Z < 2 – 3• galaxy size ~ 1 arcsecgalaxy size ~ 1 arcsec• R ~ 10000R ~ 10000• EE in H : 40% in 250 mas ~ 6 EE in H : 40% in 250 mas ~ 6 λλ/D/D• 15 to 20 objects15 to 20 objects• 25’ FoV25’ FoV

40 m class specifications40 m class specifications• Z up to Z up to 5 – 85 – 8• galaxy size galaxy size 0.15 arcsec0.15 arcsec• R ~ 10000R ~ 10000• EE in H : EE in H : 40% ??40% ?? in in 50 mas ??50 mas ??• 10 objects10 objects• 10’ FoV10’ FoV

Preliminary hints on design choices:Preliminary hints on design choices:• specs versus NGS/LGS choicespecs versus NGS/LGS choice• MOAO compared to GLAOMOAO compared to GLAO

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MOAO: impact of specificationsMOAO: impact of specifications

scientificspecification ?

Specs strong impact on limiting magnitude

H bandH band

42 m telescope ideal case: noise + fitting, no anisoplanatism… , nact > 5000 42 m telescope ideal case: noise + fitting, no anisoplanatism… , nact > 5000

LGSLGS

NGSNGS

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MOAO design issues: LGS/NGS , comparison with GLAO

GLAO

MOAO

Laser

• GLAO far below specs

• MOAO with GSs in 2 arcmin FoV meets specs

• Ideal LGS here: no elongation/cone effect

for VERY large telescopes TT not an issue

but still is for 40m-tel, 50mas resel, 50m Lo

see B. Neichel et al., IAU Le Cap, 2005 & SPIE Orlando 2006

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Results strongly dependent onResults strongly dependent onturbulence parameters:turbulence parameters:seeing, Cn2 and Lo profilesseeing, Cn2 and Lo profiles

collab. with LUAN-Nice collab. with LUAN-Nice

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MCAO: Current StatusMCAO: Current Status

• MCAO/GLAO/MOAO Concepts well established: theorerical studies, numerical simulations

• Laboratory tests are under progress at ESO, Obs. Meudon and Onera

• 10m class telescope intrumentation programmes are launched

• Next step: MCAO for ELTs– precise the scientific specifications and associated high level technical specs

– pursue design studies for MCAO/GLAO/MOAO and specify key components (DMs, WFS, LGS, control…)

– strong MOAO effort in France: ESO study MOMFIS, ELT-design-study WFSPEC

– turbulence inputs are required: Paranal campaign planned by LUAN-ESO in collab. Onera

• To know more on MCAO:Special Issue Comptes Rendus de l’Académie des Sciences, Physique Series, Dec. 2005

[articles available on ScienceDirect]

all this started with Come-On and with the VLT programme under the impulse of Pierre Lénapersonnaly: Pierre helped me set up in 1990 a pre-doc at NSO-SacPeak followed by PhD on AO co-supervised by Pierre and Gérard Rousset