E-ELT Instrumentation Project Office Adaptive Optics for the E-ELT status review of Phase A & B activities Norbert Hubin Adaptive Optics Department

E-ELT Instrumentation Project Office The Adaptive E-ELT 2 Phase “B” Design Study launched end years study Why? Increased collecting area  Fainter sources Increased diameter  Increased spatial resolution (with AO) Baseline Design 5 mirrors design 42 meters diameter cost 1000 M€

E-ELT Instrumentation Project Office Adaptive Optics Zoo GLAO-LGSLTAO: ATLASMCAO:MAORYMOAO:EAGLE 6-8 LGSs in Ø 7.2’ Few” IFU SCAO & XAO: EPICSGLAO-NGS

E-ELT Instrumentation Project Office E-ELT AO Modes Studied  #1: Seeing-limited;1’: Improved seeing  #2a: Luminosity-limited  #2b: Diffraction-limited 2b LTAO MCAO S H  30% 2b2b XAO S H  80% 1’ Multi-LGS GLAO 1 internal AO NGS 2a MOAO MCAO C H  35% 0”.1 px 0”.8 s 0 25 m L 0 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 1 st 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’’ seeing Model 2: 90% in first 500m, 0.6’’ seeing  Largest impact of all parameters for GLAO Model 3: 35% in first 500m, 1’’ seeing Model 4: 80% in first 500m, 1’’ seeing Difference between 25% best and 25% worst Paranal

E-ELT Instrumentation Project Office PSFs of GLAO Atm 1 Slide 7 KHJI GLAO seeing

E-ELT Instrumentation Project Office PSFs of GLAO Atm 2 Slide 8 KHJI GLAO seeing

E-ELT Instrumentation Project Office Limiting magnitude / Sky Coverage Slide 9 Approximate magnitude per guide star mRmR b=90°b=60°b=30°b=0° ’ FOV Numbers being cross validated with ESO astronomers Sky coverage by P. La Penna

E-ELT Instrumentation Project Office Universe expansion  cm/s V R over 20-year Exo-planet V R detection  cm/s V R over 2-year IGM low-  metallicity #1: Seeing-limited (fast aO) Light beam stabilization: T/T, focus,... optical domain CODEX (coudé Lab)  m;  ~ 1.2x10 5 ESO, Trieste & Brera, IAC, IoA, UniGe

E-ELT Instrumentation Project Office #1’: Improved Seeing (GLAO) Large Scale Structure/galaxy evolution  huge multiplex spectrometer reddish domain OPTIMOS: wide Field visual MOS (fibre or slit-based)

E-ELT Instrumentation Project Office Single Conjugate AO NGS 1 st light diffraction limited AO?  #2b: on-axis diffraction-limited  SCAO-NGS s 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 1 st light? even in degraded Sky Coverage performance SIMPLE HARMONI MICADO METIS

E-ELT Instrumentation Project Office Telescope Adaptive Optics : Deformable Mirror Instruments WFS adaptor WFS arms (contain WFS detectors) Some instruments also contain WFS detectors WFS adaptor Pupil steering mirror Field steering mirror Reimaging lens Collimator Lenslet array 1100 mm Zoom optics Detector WFS arm preliminary optical design

E-ELT Instrumentation Project Office LGS-NGS GLAO  #1’: Improved seeing  GLAO + 4 LGS [fast T/T + ~ 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 1 st level AO [mostly on] also 1 st 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 0.5 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 0.5 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 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. HubinOPTICON board meeting 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 2 nd contract at the end of 1 st contract  2 nd 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 2 nd 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: photons/m 2 /s per LGS at Nasmyth (Na column density: m -2 )  Baseline specification Emission wavelength: peak of the D 2a 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 D 2a and D 2b lines in the mesosphere The frequency shift between the two lines shall be stable within  10 MHz 18 W in the D 2a line and 2 W in the D 2b line Linewidth between 40 MHz and 250 MHz (for both lines)  Laser beam quality (long term): M 2 < 1.3 (goal 1.1)

E-ELT Instrumentation Project Office 24/14 MOAO EAGLE & MAORY MCAO  #2a: Luminosity-limited  MOAO/6-8LGS s (5-10’ field) or MCAO/6LGS s (< 2’ field)  Spaxel of 75 mas; 30% Ensquared Energy  most sky; 75% seeing (K) / very good seeing (I) 2 nd 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  m IFS LAM, 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) 2 nd 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) 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 1 st light?)  m D-L imager MPE, MPIA, USM, INAF, NOVA HARMONI (SCAO 1 st light?)  m D-L single IFU Oxford, 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 [~ modes]  also ‘visible’ AO  few 10-9 contrast so far Exo-planet direct detection  critical internal stability Debris disks 2 nd level AO [maximal Strehl] EPICS  m diff. spectro/polarimeter ESO, LAOG, LESIA, FIZEAU Lab, LAM ONERA, Oxford, Padova, ETHZ, NOVA X-AO Apodizer Differential 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 METIS L-M-N-(Q) imager/spectrometer Leiden 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 Coud è Location envisaged for CODEX with GLAO

E-ELT Instrumentation Project Office AO performance overview (preliminary) (seeing = 0.71 arcsec μm – on axis perf) AO typeNb N-LGSsStrehl(K) % EE in 75mas FWHM (mas) Sky Coverage % (60° lat.) PSF uniformity SCAO-NGS (postfocal) 1 NGS on- axis 70  mas2 anisoplanatism NGS-GLAO (Telescope) 3 NGS<0.3< good LGS GLAO (Telescope) 4LGS >4.2’ 1 NGS Very good EAGLE (Postfocal) 6-8LGSs>7.2’ 1 NGS N/A30>11100Sporadic PSF uniformity ATLAS (Postfocal) 6 LGSs>4.2’ 2 IR NGSs anisoplanatism MAORY (postfocal) 2’ 3 IR NGSs Excellent EPICS1NGS on axis90 in HFew 10-9 contrast 11Set 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 2 nd 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 1 st 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 elongation Perspectives for tomography: comparison of metapupils 3 LGS Central launch3 LGS Side launch less elongation where seen only once Side launch solution open options to use Fractal iterative method to further reduce the laser flux requirement  study on-going for MCAO as seen at 10 km altitude

E-ELT Instrumentation Project Office LGS : 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