Adaptive Optics for the E-ELT status review of Phase A & B activities

E-ELT Instrumentation Project Office

Adaptive Optics for the E-ELTstatus review of Phase A & B activities

Norbert HubinAdaptive Optics Department


The Adaptive E-ELT

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Phase “B” Design Study launched end 2006 - 3 years study

Why?Increased collecting area Fainter sourcesIncreased diameter Increased spatial resolution (with

AO)

Baseline Design• 5 mirrors design• 42 meters

diameter• cost 1000 M€


Adaptive Optics ZooGLAO-LGS LTAO: ATLAS MCAO:MAORY MOAO:EAGLE

6-8 LGSs in Ø 7.2’

Few” IFU

SCAO & XAO: EPICS

GLAO-NGS


E-ELT AO Modes Studied #1: Seeing-limited;1’: Improved seeing #2a: Luminosity-limited #2b: Diffraction-limited

2bLTAOMCAO SH

30%2b

XAO SH 80%

1’Multi-LGSGLAO1 internal AO

NGS

2aMOAOMCAO

CH 35%0”.1 px

• 0”.8 s0• 25 m L0

H-band

240 mas

H-band

800

mas

400 mas

H-band

8/100 mas

Combined Telescope – AO Systems – Instrument capability


5/14

GLaO NGS #1: Seeing-limited

3 NGS GLAO [active optics + 10Hz TT ~few 100 low order aberrations incl. phase error propagation] all clear/safe nights; whole sky; 10’ field; all

1st level fast aO [always on]


Impact of Cn2 profile (5’ FOV)

Slide 6

Model 1: 46 % in first 500m, 0.6’’ seeingModel 2: 90% in first 500m , 0.6’’ seeing

Largest impact of all parameters for GLAO

Model 3: 35% in first 500m, 1’’ seeingModel 4: 80% in first 500m , 1’’ seeing

Difference between 25% best and 25% worst profiles @ Paranal


PSFs of GLAO Atm 1

Slide 7

K H J I

GLAO

seeing


PSFs of GLAO Atm 2

Slide 8

K H J I

GLAO

seeing


Limiting magnitude / Sky Coverage

Slide 9 Approximate magnitude per guide star

mR b=90° b=60° b=30° b=0°12 0.00 0.00 0.00 0.0013 0.00 0.00 0.00 0.0014 0.00 0.00 0.01 0.6315 0.02 0.05 0.22 1.0016 0.13 0.19 0.69 1.0017 0.39 0.46 0.95 1.0018 0.70 0.75 1.00 1.0019 0.92 0.93 1.00 1.0020 0.99 0.99 1.00 1.00

5’ FOV

Numbers being cross validated with ESO astronomers

Sky coverage by P. La Penna


• Universe expansion cm/s VR over 20-year

• Exo-planet VR detection cm/s VR over 2-year

• IGM low- metallicity

#1: Seeing-limited (fast aO)

Light beam stabilization: T/T, focus, ...

optical domain

CODEX (coudé Lab)0.37--0.69+ m; ~1.2x105

ESO, Trieste & Brera, IAC, IoA, UniGe


#1’: Improved Seeing (GLAO)

• Large Scale Structure/galaxy evolution

huge multiplex spectrometerreddish domain

OPTIMOS: wide Field visual MOS (fibre or slit-based)


Single Conjugate AO NGS 1st light diffraction limited AO?

#2b: on-axis diffraction-limited SCAO-NGSs a la NACO(< 1’ field); variable PSF Visible & IR Wavefront sensor for highly obscured region 70-45% Strehl ratio in K; 80% EE in 75mas spaxel 11 mas FWHM, low sky coverage<2%

Any instrument using AO at 1st light? even in degraded Sky Coverage performance• SIMPLE• HARMONI• MICADO• METIS

E-ELT Instrumentation Project OfficeTelescope Adaptive Optics

: Deformable Mirror

Instruments

WFS adaptor

WFS arms (contain WFS detectors)

Some instruments also contain WFS detectors

WFS adaptor

09:56:46

Position: 1 28-Apr-09

180.00 MM

Pupil steering mirror

Field steering mirror

Reimaging lens

Collimator

Lenslet array

1100 mm

Zoom optics

Det

ecto

r WFS arm preliminary optical design


LGS-NGS GLAO #1’: Improved seeing

GLAO + 4 LGS [fast T/T + ~5.103 modes]; 250 mas FWHM or with 3 NGS [30-50% sky in K; laser-adverse nights] no/light* cirrus; ~ all seeing; ~ full sky in J-H-K

5’ field in K; ~40” at 600 nm - limited sky coverage

1st level AO [mostly on]

also 1st step to MCAO, MOAO & XAO


Number of LGSs for GLAO ?

Slide 15 Old simulation conditions, so EE values should be scaled


One possible M4 Adaptive Mirror

May 12th, 2009 E-ELT Phase B Mid-term Review 16

• 7k actuators WFE=113 nm rms (seeing 0.85” @ 0.5 μm

• Full stroke of 80 μm• Mirror positioned with a hexapod


Another possible M4 unit

E-ELT Mid-term review - May 2009 Slide 17

Shell machining• 6k actuators

WFE=129 nm rms (seeing 0.85” @ 0.5 μm

• Full stroke of 160 μm• Mirror positioned with a

hexapod + Nasmyth switcher


Mounting frame

Backside with support elements and actuators

A possible 2.6m M5 field stabilization Unit


• 40 cm Laser launch Telescope

• Up to 2x20W laser unit each• Relay, diagnostic tools• Jitter, beam steering• Enclosed baffle?• LGS station access &

servicing

Laser Guide Star Concept: side launch


Side launching fratricide effect (LGS beacons rotating with sky field)

E-ELT BRDv3 Nov 2008 Slide 20

GLAO WFSs with 4LGSs

MOAO WFSs with 6 LGSs


E-ELT launch telescope baseline VLT AOF• Diameter: 400mm• Useful aperture: 300mm• Unvignetted Fov: 12’• Pointing precision: <0.1”• Output Beam diameter 300 mm• Beam magnification 20• WFE excluded focus: 50nm rms• Focus WFE: <1 wave P-V

at 589nm• Throughput @ 589nm: T ≥ 95%• Total max: <200kg• Interface: TBD

4 units being designed & built by TNO-TPD (NL) for VLT-AOF


N. Hubin

OPTICON board meeting 11.08

Sodium Laser studies: AOF E-ELT?

1st contract: PDR and Critical Technology Demonstrator development Goal: to secure interfaces and critical technology (risk reduction) 2 studies & 2 risk reduction studies funded by (ESO, OPTICON) &

(Keck, TMT, GMT & AURA) Fasortronic (USA) & TOPTICA (GER): both have demonstrated >20W Feb.- Nov 2009 Firm fixed price offer for 2nd contract at the end of 1st contract

2nd contract: FDR & Pre-Production Unit (2010) Final Design Phase: 6 months (incl. long lead items procurement) Pre-Production Unit MAIT: 12 months

After go-no go milestone 2nd contract: MAIT and delivery of 4 Laser Units Laser Units MAIT and delivery: 17 months


Sodium Laser Requirements

CW or QCW laser Return flux: 4-5 106 photons/m2/s per LGS at Nasmyth (Na column

density: 4 1013 m-2) Baseline specification

Emission wavelength: peak of the D2a line in the mesosphere (≈589 nm)

25 W - line width = 50 MHz 10 MHz Optional specification: making use of Sodium back-pumping!

2 lines emitted: peak of D2a and D2b lines in the mesosphere The frequency shift between the two lines shall be stable within 10

MHz 18 W in the D2a line and 2 W in the D2b line Linewidth between 40 MHz and 250 MHz (for both lines)

Laser beam quality (long term): M2 < 1.3 (goal 1.1)


24/14

MOAO EAGLE & MAORY MCAO #2a: Luminosity-limited

MOAO/6-8LGSs (5-10’ field) or MCAO/6LGSs (< 2’ field)Spaxel of 75 mas; 30% Ensquared Energy most sky; 75% seeing (K) / very good seeing (I)

2nd level AO [photon-starved]

• Physics & mass assembly of galaxies to z

~4.7 highest H-K energy concentration (30%) in 75 mas

• Highest redshift galaxies at z > 6 highest patrol field (up to 10’ with MOAO)EAGLE

0.8-2.4 m 20+-IFSLAM, OPM, ONERA, UKATC, Durham


25/14

MCAO MAORY & LTAO ATLAS #2b: Diffraction-limited

60% sky coverage & 50% seeing in K, Strehl(K)>40-50% 15% sky & exceptional seeing in I ATLAS/6LGSs(15-30”field) & MAORY/6LGSs (< 2’ field)

2nd level AO [maximal resolution]

MAD ‘06

Ω Cen


• resolved stellar population imaging 1% photometric precision CMD in K-I

• resolved stellar population spectroscopy good Strehl at 850 nm (Ca Triplet)

• Z~2-5 L* galaxy imaging very low-noise science detector

• SMBH spectroscopy at center of galaxies extremely low-noise science detector

#2b: Diffraction-Limited (MCAO/LTAO)

MICADO (SCAO 1st light?)0.8-2.4 m D-L imagerMPE, MPIA, USM, INAF, NOVA

HARMONI (SCAO 1st light?)0.8--2.4 m D-L single IFUOxford, CRAL, DAMI. UKATC

ATLAS


EPICS: XAO & high contrast

#2b: Extreme contrast 25% seeing; zero field; 0.65 μm XAO/NGS [~3.104 modes] also ‘visible’ AO few 10-9 contrast so far

• Exo-planet direct detectioncritical internal stability

• Debris disks

2nd level AO [maximal Strehl]

EPICS0.6-1.8 m diff. spectro/polarimeter ESO, LAOG, LESIA, FIZEAU Lab, LAM ONERA, Oxford, Padova, ETHZ, NOVA

X-AOApodizerDifferential extraction


LTAO ATLAS & SCAO Mid-IR AO (8-24 μm)

M4-M5 provides ATLAS/SCAO NGS on 60% sky (0.9 Strehl) (IR WFS for highly obscured regions) ~ luminosity / diffraction-limited

• Circumstellar dust chemistry PaH spectrometry (high-sensitivity N detector)

• Planet-forming dust emission

METISL-M-N-(Q) imager/spectrometerLeiden et al.


A POSSIBLE AO & INSTRUMENT DISTRIBUTION (Nasmyth)

Test Camera

OPTIMOS

MAORY

MCAO module

MICADO

SCAO, LTAO module

HARMONI

METIS

EPICS+ XAO

E-ELT Instrumentation Project Office A POSSIBLE INSTRUMENT DISTRIBUTION (GI & coudé)

LTAO module

Adaptor, GI feeding unit

P

HARMONI

METIS

EPICS+ XAO

P

LTAO

GI Location envisaged EAGLE with MOAO & SIMPLE with SCAO or LTAO

Coudè Location envisaged for CODEX with GLAO


AO performance overview (preliminary)(seeing = 0.71 arcsec -- perf @ 2.2 μm – on axis perf)

AO type Nb N-LGSs Strehl(K) % % EE in 75mas

FWHM(mas)

Sky Coverage % (60° lat.)

PSF uniformity

SCAO-NGS(postfocal)

1 NGS on-axis

70 45 80 11 mas 2 anisoplanatism

NGS-GLAO(Telescope)

3 NGS <0.3 <8-9 250 50 good

LGS GLAO(Telescope)

4LGS >4.2’1 NGS

0.3 8-9 250 100 Very good

EAGLE(Postfocal)

6-8LGSs>7.2’1 NGS

N/A 30 >11 100 Sporadic PSF uniformity

ATLAS(Postfocal)

6 LGSs>4.2’2 IR NGSs

55 64 11 60 anisoplanatism

MAORY(postfocal)

6LGSs @ 2’3 IR NGSs

50 58 11 60 Excellent

EPICS 1NGS on axis 90 in H Few 10-9 contrast

11 Set of targets

N/A

Inputs from T. Fusco


E-ELT AO Requirements?

A permanent Internal AO capability (NGSs) to get decent images at all + MIR D-L SCAO

Giving a GLAO-based correction (+ LGSs) most of the sky & time [cirrus/lasers permitting] also LTAO for small field/high sky coverage near D-L

Often with an instrument-related 2nd AO stage wide patrol-field spectroscopy (MOAO/MCAO) diffraction-limited (spectro)-imagery (MCAO) extreme-contrast (spectr./polar.)-imagery (XAO)

Pushing the envelope on every aspect Strehl; energy concentration, sky coverage, , ... but also photometry, stability, astrometry, contrast ....


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Thank you for your patience!Thank you also to the whole

European AO community for the hard work so far!!!


E-ELT Adaptive Optics overview• Telescope AO: with M4 & M5 correctors + LGSF

– Ground Layer AO with 3 NGSs– Ground Layer AO with 4 LGSs– Engineering Single Conjugate AO

• Postfocal AO: M4 & M5 units as 1st stage correctors– Laser Tomography AO Module: ATLAS– Multi-Conjugate AO Module: MAORY– Multi-Object AO integrated into EAGLE– Extreme AO integrated into EPICS (NGS)– Single Conjugate AO using IR WFS integrated into MIDIR

(NGS+ LGS)– Single Conjugate AO using Vis WFS integrated into

instruments (TBC)34


On-going research work to reduce spot elongationPerspectives for tomography: comparison of metapupils

3 LGS Central launch 3 LGS Side launch

less elongationwhere seen only once

Side launch solution open options to use Fractal iterative methodto further reduce the laser flux requirement study on-going for MCAO

as seen at 10 kmaltitude

E-ELT Instrumentation Project OfficeLGS : choice of a launching scheme

Spot elongation and noise propagation • Spot elongation and noise propagation

E2E simulation . Telescope = 21m. Scaling factors 6 LGS position : 1 min ring Representative of 42 m

Tomographic performance M1 ≡ M2

Even a small gain from a pure performance point of view !

More uniform propagation onto modes !

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Adaptive Optics for the E-ELT status review of Phase A & B activities

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