MOAO description MOAO on the E-ELT CANARY Phase A System calibration On-sky results CANARY Phase B

Multiple Object Adaptive Optics A technique for extending Adaptive Optics

correction to multiple objects distributed within a very wide field of regard

Planned operating mode for several facility class instruments: RAVEN on Subaru CONDOR on the VLT Keck NGAO NFIRAOS on TMT EAGLE on the E-ELT

10’ Technical

5’ Science

SCAO/LTAO/XAO

MCAO

GLAO

MOAO

E-ELT focal plane

SCIENCE

CAMERA

WFS 2WFS 1

ATM

OS

PH

ER

IC

TU

RB

ULEN

CE

ATM

OS

PH

ER

IC

TU

RB

ULEN

CE

TELESCOPE PUPIL

SCIENCE

CAMERA

WFS 2WFS 1

Tomographic Wavefront Sensing

Tomographic Wavefront Sensing

Tomographic Wavefront Sensing

Closed-loop wavefront control (MCAO)

Wide field of view allows the WFSs to be positioned behind the DM

ABERRATED WAVEFRON

T

DEFORMABLE

MIRROR(S)

WFSS

CORRECTED

WAVEFRONT

SCIENCE CAMERA/IF

U

Closed-loop wavefront control (MCAO)

Optimal correction FOV of an MCAO system

ABERRATED WAVEFRON

T

DEFORMABLE

MIRROR(S)

WFSS

CORRECTED

WAVEFRONT

SCIENCE CAMERA/IF

U

Open-loop wavefront control (MOAO)

WFS and science paths are separated. WFSs cannot observe the AO correction

ABERRATED WAVEFRON

T

DEFORMABLE

MIRROR(S)WFSS

CORRECTED

WAVEFRONT

SCIENCE CAMERA/IF

U

EAGLE is a proposed MOAO IFU spectrograph for the E-ELT 20 IFU channels with a

1.6” FOV and 35mas sampling

EAGLE will provide ≥30% EE within 70mas at 1.6µm

Two modes providing R=4000 & 10000 Phase A EAGLE design

installed in the GIFS of the E-ELT

LTAO/SCAO Excellent correction Too slow to perform surveys

with only a single IFU MCAO

Very good correction Too many DMs required to reach

performance requirements over full FOV

GLAO Very wide field, minimal

correction Performance is low and highly

dependent on turbulence profile MOAO

Distributed open-loop AO with integrated multi-IFU system

One DM per target field means optimal correction along every line of sight

Performance and sky coverage means LGS

5 main science cases: The evolution of distant galaxies Detection and characterisation of first-light

galaxies at the highest redshifts The physics of galaxy evolution from stellar

archaeology Star-formation, clusters, and the initial mass

function Co-ordinated growth of black holes and

galaxies in the local and distant Universe Many more auxiliary science cases All benefit from the multiplex over

observing 20 patches of sky at once...

9 arcsec

ACS image

ACS image

Simulated EAGLE cube

I = 22.5 S/N=43 & 36

I = 23.1 S/N=23

I = 22.8 S/N=28

EAGLE: 1000 stars in ~ 25 hrs

1.6’’ x 1.6’’

VOLT 1 and ViLLaGEs 2 have both demonstrated open-loop AO on-sky

Tomographic MOAO had never been demonstrated on-sky Neither NGS or LGS tomography

Several questions left to answer for MOAO & EAGLE: Accuracy of tomographic wavefront sensing and

reconstruction Open-loop DM control Required calibration and alignment procedures Closed-loop woofer/open-loop tweeter DM

configuration Sensitivity to changing turbulence profiles …

1 Andersen et al, Proc SPIE 7015, 70150H (2008)2 Morzinski et al, Proc SPIE 7736, 77361O (2010)

Create a single MOAO channel EAGLE as closely as possibly using the 4.2m William Herschel Telescope Effectively a 1/10th scale model of E-ELT using a

10km Rayleigh LGS

Perform NGS, then LGS based tomographic WFSing

Perform open-loop AO correction on-sky Develop calibration and alignment techniques Fully characterise system and subsystem

performance No requirement to perform astronomical

science…

13th October 2009 CANARY: An LGS MOAO demonstrator

Components: Low-order 8x8 DM 3 x L3CCD open-loop NGS WFSs Open-loop optimised Fast

Steering Mirror Hardware accelerated Real

Time control system NGS MOAO Calibration Unit

WHTNasmyth

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

NGS WFS

NGS WFS

NGS WFS

10" science FOV

2.5’ Derotated WHT field

Telescope Simulator not shown, but it feeds in here

• PC based• Runs as a multi-threaded high

priority process• Compatible with real-time Linux

• Modular design• Shared memory telemetry

interface• System controlled via CORBA

object• Updates at ~1.2kHz with CPU

pixel processing• ~5kHz with FPGA pixel processing

• Measured latency of 0.8ms• Robust operation• Open-source…

CANARY contains over 20 calibration and alignment sources

4 x off-axis VIS SL sources4 x off-axis VIS DL sources1 x on-axis VIS SL source1 x on-axis VIS DL source1 x on-axis NIR DL source

1 x on-axis alignment laser1 x on-axis pupil alignment laser1 x on-axis pupil pinhole source1 x on-axis NIR DL source1 x on-axis VIS SL source1 x on-axis VIS DL source1 x off-axis source for figure sensor

1 x on-axis VIS SL source1 x on-axis reverse path source

Open-loop WFSs measure the DM response by looking backwards through the AO system

The reverse-path interaction matrices contain all NGS WFS – DM registration information

AO PATH

WFS

Input Focal Plane

Output Focal Plane

Learn and Apply calibration procedure Record 10-30s of on-sky wavefront data from the

on- and off-axis WFSs Calculate a turbulence profile from this data Calculate covariance matrices between off-axis

WFSs using the fitted profile and asterism parameters

Calculate covariance matrices between on and off-axis WFS

Additional steps to remove static telescope aberrations, errors due to telescope tracking updates, pupil conjugation, rotations etc.

4 LGS and 2 NGS Phase B LGS example…

LGS//LGSLGS//LGS

LGS//NGS_TTLGS//NGS_TT

NG

S_T

T //LG

SN

GS_T

T //LG

S

NGS_TT//NGS_TT//NGS_TTNGS_TT

LGS//NGSLGS//NGS

NG

S//LG

SN

GS//LG

S

NGS//NGS//NGSNGS

NG

S//

NG

S//

NG

S_T

TN

GS

_TT

NGS_TT//NGS_TT//NGSNGS

COffOffCOnOff-1x=Mt -1

= x

TS//TS//LGSLGS

TS//TS//NGS_TNGS_TTT

TS//TS//NGSNGS

high high ordeorderr

TT onlyTT only

HO + HO + TTTT

52

72

72

x6

72

+2

Mt TS Control matrixx

x

=Mct(Measured in lab)

=

54

72

x6

8 nights allocated on the WHT 4 in September 2010, 4 in November 6 nights lost to bad weather!

3 asterisms observed

Initial results only

Much more analysis required to fully understand the system

H-band 2 x 2” FOV 30s exposures

seeing ≈3% GLAO 13%

SCAO 27% MOAO 25%

from nightSept. 27-28

SCAO = ▲ MOAO = ◯GLAO = ◻

from nightSept. 27-28

SCAO = ▲ MOAO = ◯GLAO = ◻

Sometimes there is little difference between GLAO and MOAO

Some of the performance variation is due to parameter tuning within the RTCS (gain, thresholds etc.)

The small aperture of the WHT limits CANARY tomography to altitudes below ~6km Precise value dependent on asterism parameters

and reconstruction Tomography would work better on a larger

telescope Increase in pupil diameter from 4m to 8m will push

performance closer to SCAO levels LGS are necessary to get sky coverage anyway

from nightSept. 27-28

PessimisticapproximationSR=exp(-σ2)SCAO = ▲

MOAO = ◯GLAO = ◻

Performance at the lowest spatial frequencies does not match theory Similar characteristics observed with both VOLT and

ViLLaGEs Several possible explanations still under

investigation Best optical performance of the system is

~70% in the H-band DM surface exhibits high-frequency polishing errors?

Throughput to NGS WFSs is lower than expected Issue with the frame transfer?

•Tomographic MOAO demonstration•Open-loop GLAO demonstration•MMSE Tomographic reconstructor •Learn & Apply tomographic calibration•Additional demonstrations:

• New Shack-Hartmann WFSing algorithms:• Brightest pixel centroiding, adaptive windowing,

correlation (and more)• New type of polarisation based WFS (YAW/ADONF)• On-sky measurement of interaction matrices• CPU-based (Linux) Real Time Control system• FPGA and GPU RTC acceleration

Adds four open-loop LGS WFSs to the existing three NGS WFSs

Can run in LGS or NGS modes or a mixture of both

Crucial for demonstrating EAGLE

WHTNasmyth

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

LGSFSM

LGS Dichroic

Phase B: Low-order LGS MOAO

LGS WFS

1.0’ Diameter LGS asterism

The relay optics are designed to transport the full 3’ diameter FOV – required for Phase C

Only the central 10’’ is actuallyused by the camera

focalplane

copy of thefull focal plane

NGSwfs

telescope rotater

NGSwfs

AdonisDM camera

relay optics

We have done this at Phase A:

telescope rotaterAdonis

DM camera

relay optics

We planned to do this:

NGSwfs

NGSwfs

dichro

LGSwfs

dichro

LGSwfs

NGSwfs

telescope rotater

NGSwfs

AdonisDM camera

relay optics

But ended up designing this so we could fall back to Phase A:

This layout is complicated by the crowded focal plane.....

LGS beam separated dichroically before NGS WFSs

LGS WFS positioned on raised bench

MIT/LL CCID-18 electronically gated CCD

LGS Tip/tilt mirror to correct for LGS launch jitter

Only have a single detector and we need to place 4 SH WFS patterns on it

Designed a pyramid prism to allow us to vary LGS asterism altitude and spacing

• Altitude range: 11 km to 25 km

• Asterism range: LGS diagonal on sky between 3.2 m and 3.8 m

Change the asterism altitudeChange the asterism diameter

Laser enclosure mounted at the top-ring of the telescope

2 x 16W lasers are combined and then sent through a DOE to create the 4 LGS asterism

Interfaces to existing WHT beam-launch optics

Multi-LGS system being commissioned in July/November

Phase B CANARY being commissioned in Paris

On-sky date for full Phase B system of May 2012

Image of 4 LGS asterism taken during testing in

2008

WHT Rayleigh LGS, GLAS, being launched during 2008

CANARY lasers during acceptance testing at Durham (2010)

MOAO is a powerful technique for extending high accuracy AO correction to points distributed over a very wide field

CANARY has demonstrated fully tomographic NGS MOAO on-sky

Tomographic reconstruction achieved significant improvement over GLAO, and approached SCAO levels of performance

Initial results promising, but more work is required to fully understand results

LGS upgrade is progressing and will be commissioned in July

It has been a very easy to integrate and test new hardware and software modules into CANARY in addition to demonstrating MOAO

AO4ELTs, Paris 2009 CANARY: NGS/LGS MOAO demonstrator

DurhamDurham Richard Myers, Gordon Talbot, Nigel Dipper, Deli Geng, Eddy Younger, Richard Myers, Gordon Talbot, Nigel Dipper, Deli Geng, Eddy Younger, Alastair Basden, Colin Dunlop, Nik Looker, Jonny Taylor, Tim Butterley, Alastair Basden, Colin Dunlop, Nik Looker, Jonny Taylor, Tim Butterley, Laura Young, Simon Blake, Sofia Dimoudi, Paul ClarkLaura Young, Simon Blake, Sofia Dimoudi, Paul Clark

Obs. ParisObs. Paris Zoltán Hubert, Gerard Rousset, Eric Gendron, Fabrice Vidal, Damien Zoltán Hubert, Gerard Rousset, Eric Gendron, Fabrice Vidal, Damien Gratadour, Aglae Kellerer, Michel Marteaud, Fanny Chemla, Phillipe Laporte, Gratadour, Aglae Kellerer, Michel Marteaud, Fanny Chemla, Phillipe Laporte, Jean-Michel Huet, Matthieu BrangierJean-Michel Huet, Matthieu Brangier

UKATCUKATC Andy Longmore, David Henry, Stephen Todd, Colin Dickson, Brian Stobie, Andy Longmore, David Henry, Stephen Todd, Colin Dickson, Brian Stobie, David AtkinsonDavid Atkinson

ONERAONERA Thierry Fusco, Clelia Robert, Nicolas Vedrenne, Jean-Marc ConanThierry Fusco, Clelia Robert, Nicolas Vedrenne, Jean-Marc Conan

INGING Jure Skvarc, Juerg Rey, Neil O’Mahoney, Tibor Agocs, Diego CanoJure Skvarc, Juerg Rey, Neil O’Mahoney, Tibor Agocs, Diego Cano

PUC SantiagoPUC Santiago Andres Guesalaga, Dani GuzmanAndres Guesalaga, Dani Guzman

L2TIL2TI Caroline Kulscar, Gaetano Sevo, Henri-Francois RaynaudCaroline Kulscar, Gaetano Sevo, Henri-Francois Raynaud

Engineering and Project Engineering and Project Solutions LtdSolutions Ltd

Kevin DeeKevin Dee

The CANARY project is supported via the following funding bodiesThe CANARY project is supported via the following funding bodies STFCSTFC UK E-ELT Design StudyUK E-ELT Design Study EU FP7 Preparatory fund WP9000EU FP7 Preparatory fund WP9000 ANR Mauii, INSU, Observatoire de ParisANR Mauii, INSU, Observatoire de Paris FP7 OPTICON JRA1FP7 OPTICON JRA1