1. AO4ELT, Paris, 23 June 2009 EPICS, exoplanet imaging with the E-ELT Markus Kasper, Jean-Luc Beuzit, Christophe Verinaud, Emmanuel Aller- Carpentier, Pierre Baudoz, Anthony Boccaletti, Mariangela Bonavita, Kjetil Dohlen, Raffaele G. Gratton, Norbert Hubin, Florian Kerber, Visa Korkiaskoski, Patrice Martinez, Patrick Rabou, Ronald Roelfsema, Hans Martin Schmid, Niranjan Thatte, Lars Venema, Natalia Yaitskova ESO, LAOG, LESIA, FIZEAU, Osservatorio Astronomico di Padova, ASTRON, ETH Zürich, University of Oxford, LAM, NOVA 1 1

2. AO4ELT, Paris, 23 June 2009 Outline  Science goals (6s)  Instrument and AO concept (12s)  Science Output prediction (4s) 2

3. AO4ELT, Paris, 23 June 2009 Exoplanets observations early 2009 3  ~ 300 Exoplanets detected, >80% by radial velocities, mostly gas giants, a dozen Neptunes and a handful of Super-Earths  Constraints on Mass function, orbit distribution, metallicity  Some spectral information from transiting planets Spectrum of HD 209458b Richardson et al., Nature 445, 2007 3 HR 8799, Marois et al 2008Beta Pic, Lagrange et al 2009

4. AO4ELT, Paris, 23 June 2009 (Some) open issues 4  Planet formation (core accretion vs gravitational disk instability)  Planet evolution (accretion shock vs spherical contraction / “hot start”)  Orbit architecture (Where do planets form?, role of migration and scattering)  Abundance of low-mass and rocky planets  Giant planet atmospheres 4

5. AO4ELT, Paris, 23 June 2009 Object Class 1, young & self-lum Planet formation 5 in star forming regions or young associations Requirements: High spat. resolution of ~30 mas (3 AU at 100 pc, snow line for G-star ) Moderate contrast ~10 -6 5

6. AO4ELT, Paris, 23 June 2009 Object Class 2, within ~20 pc Orbit architecture, low-mass planet abundance 6 ~500 stars from Paranal ± 30 deg, ~60-70% M-dwarfs Requirements High contrasts ~10 -9 at 250 mas (Jupiter at 20pc) + spatial resolution ~10 -8 at 40 mas (Gl 581d,~8 M  ) 6

7. AO4ELT, Paris, 23 June 2009 7 Object Class 3, already known ones Planet evolution and atmospheres discovered by RV, 8-m direct imaging (SPHERE, GPI) or astrometric methods (GAIA, PRIMA) SPHERE discovery space GAIA discovery space From ESO/ESA WG report 7

8. AO4ELT, Paris, 23 June 2009 Contrast requirements summary 8

9. AO4ELT, Paris, 23 June 2009 Concept 9 9

10. AO4ELT, Paris, 23 June 2009 Concept: Achieve very high contrast Highest contrast observations require multiple correction stages to correct for 1. Atmospheric turbulence 2. Diffraction Pattern 3. Quasi-static instrumental aberrations XAO Visible diffraction suppression Diff. Pol. IFS Coherence- based concept? XAO, S~90% Diffraction + static aberration correction Speckle Calibration, Differential Methods Contrast ~ 10 -3 -10 -4 Contrast ~ 10 -6 Contrast ~ 10 -9 x 1000 ! 10 NIR diffraction suppression

11. AO4ELT, Paris, 23 June 2009 XAO concept Main parameters (baseline)  Serial SCAO M4 / internal WFS, XAO  XAO: roof PWS at 825 nm, 3 kHz  200x200 actuators (20 cm pupil spacing) 11 11 RTC requirements: Efficient algorithms studied outside EPICS phase-A Numerical simulation, see poster of Visa Korkiakoski AO + coro 1e-6 1e-7

12. AO4ELT, Paris, 23 June 2009 High Order Testbench (HOT) Demonstrate XAO / high contrast concepts  Developed at ESO in collaboration with Arcetri and Durham Univ.  Turb. simulator, 32x32 DM, SHS, PWS, coronagraphy, NIR camera  H-band Strehl ratios ~90% in 0.5  seeing (SPIE 2008, Esposito et al. & Aller-Carpentier et al. ) correcting 8-m aperture for ~600 modes See poster of Aller-Carpentier

13. AO4ELT, Paris, 23 June 2009 HOT: XAO with APL coronagraph 13  700K object next to K0 star Good agreement with SPHERE simulations Additional gain by quasi-static speckle calibration (SDI, ADI)

14. AO4ELT, Paris, 23 June 2009 HOT speckle stability 14 0+ 6hrs+30 hrs

15. AO4ELT, Paris, 23 June 2009 Correction of quasi-static WFE incl. segments piston Standard WFE specs ok for most optics (near pupil)  DM “cleans” its control area from speckles  Need: measure static aberrations some nm level at science wavelength through residual turbulence (PD or Speckle Nulling) Concept to be demonstrated  FP7 funded exp. (FFREE@LAOG and HOT) 15

16. AO4ELT, Paris, 23 June 2009 HOT: Segments piston and correction of quasi-static WFE With segmentation HOT pupil with DM and segmentation

17. AO4ELT, Paris, 23 June 2009 Residual PSF calibration Getting from systematic PSF residuals (10 -6 -10 -7 ) to 10 -8 -10 -9  Spectral Devonvolution (Sparks&Ford, Thatte et al.), Trade-off: spectral bandwidth vs inner working angle,  IFS (baseline Y-H)  Multi-band spectral or polarimetric differential imaging for smallest separation, needs planet “feature” (e.g. CH 4 band, or polarization)  IFS and differential polarimeter (600-900 nm)  Coherence based methods (speckles interfere with Airy Pattern, a planet does not)  Self-Coherent camera (see talk by P. Baudoz)  Angular Differential Imaging (ADI)  All 17

18. AO4ELT, Paris, 23 June 2009 Example: Spectral Deconvolution 18 18

19. AO4ELT, Paris, 23 June 2009 Speckle chromaticity and Fresnel 19 20 nm rms at 10x Talbot 20 nm rms in pupil plane SD needs “smooth” speckle spectrum -> near-pupil optics

20. AO4ELT, Paris, 23 June 2009 End-2-end analysis Apodizer only leads to improved final contrast APLC Apodizer

21. AO4ELT, Paris, 23 June 2009 E-ELT WFE requirements  Segment alignment (PTT) < 36 nm rms  Segment figuring < 50 nm rms  Segment high orders < 50 nm rms  M2-5, f>50 cycles/pupil< 30 nm rms  Roughness < 5 nm rms

22. AO4ELT, Paris, 23 June 2009 Baseline Concept All optics near the pupil plane minimize amplitude errors and speckle irregular chromaticity

23. AO4ELT, Paris, 23 June 2009 Detection rates, MC simulation 23 23

24. AO4ELT, Paris, 23 June 2009 Predicted Science Output MC simulations  planet population with orbit and mass distribution from e.g. Mordasini (2007)  Model planet brightness (thermal, reflected, albedo, phase angle,…)  Match statistics with RV results Contrast model  Analytical AO model incl. realistic error budget  Spectral deconvolution  No diffraction or static WFE  Y-H, 10% throughput, 4h obs 24

25. AO4ELT, Paris, 23 June 2009 Detection rates, nearby+young stars Mordasini et al. 2007 Contrast requirements 25

26. AO4ELT, Paris, 23 June 2009 Predicted EPICS output 26 Target class # targets Self- luminous planets Giant planets Neptunes Rocky planets 1. Young stars 688~100(~100)DozensVery few (?) 2. Nearby stars 512Dozen~100DozensDozen 3. Stars w. planets >100Some>100>Dozen>2 26

27. AO4ELT, Paris, 23 June 2009 Summary  EPICS is the NIR E-ELT instrument for Exoplanet research  Phase-A to study concept, demonstrate feasibility by prototyping, provide feedback to E-ELT and come up with a development plan  Conclusion of Phase-A early 2010  Exploits E-ELT capabilities (spatial resolution and collecting power) in order to greatly advance Exoplanet research (discovery and characterization) 27

28. AO4ELT, Paris, 23 June 2009 END 28 28