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Adaptive Optics for the E-ELT status review of Phase A & B activities. Norbert Hubin Adaptive Optics Department. The Adaptive E-ELT. Why? Increased collecting area Fainter sources Increased diameter Increased spatial resolution (with AO). Baseline Design 5 mirrors design - PowerPoint PPT Presentation
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E-ELT Instrumentation Project Office
Adaptive Optics for the E-ELTstatus review of Phase A & B activities
Norbert HubinAdaptive Optics Department
E-ELT Instrumentation Project Office
The Adaptive E-ELT
2
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€
E-ELT Instrumentation Project Office
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 Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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]
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
PSFs of GLAO Atm 1
Slide 7
K H J I
GLAO
seeing
E-ELT Instrumentation Project Office
PSFs of GLAO Atm 2
Slide 8
K H J I
GLAO
seeing
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
• 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
E-ELT Instrumentation Project Office
#1’: Improved Seeing (GLAO)
• Large Scale Structure/galaxy evolution
huge multiplex spectrometerreddish domain
OPTIMOS: wide Field visual MOS (fibre or slit-based)
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
Number of LGSs for GLAO ?
Slide 15 Old simulation conditions, so EE values should be scaled
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
Mounting frame
Backside with support elements and actuators
A possible 2.6m M5 field stabilization Unit
E-ELT Instrumentation Project Office
• 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
E-ELT Instrumentation Project Office
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 Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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)
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
• 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
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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.
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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 Instrumentation Project Office
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 ....
E-ELT Instrumentation Project Office
33
Thank you for your patience!Thank you also to the whole
European AO community for the hard work so far!!!
E-ELT Instrumentation Project Office
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
E-ELT Instrumentation Project Office
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 !
36