EPICS, exoplanet imaging with the E-ELT

1. EPICS, exoplanet imaging with the E-ELT Raffaele G. Gratton,Markus Kasper (PI), Jean-Luc Beuzit, Christophe Verinaud, Emmanuel Aller-Carpentier, Pierre Baudoz, Anthony Boccaletti, Mariangela Bonavita, Kjetil Dohlen,, 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, INAF-Osservatorio Astronomico di Padova, ASTRON, ETH Zürich, University of Oxford, LAM, NOVA 1

2. Outline Science goals Instrument and AO concept Science Output prediction

3. Exoplanets observations 2009 Spectrum of HD 209458b Richardson et al., Nature 445, 2007 • Close to 400 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 HR 8799, Marois et al 2008 Beta Pic, Lagrange et al 2009 3

4. (Some) open issues • 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. Object Class 1, young & self-lumPlanet formation • in star forming regions or young associations • Requirements: • High spatial resolution of ~30 mas (3 AU at 100 pc, snow line for G-star) • Moderate contrast ~10-6 5

6. Object Class 2, within ~20 pcOrbit architecture, low-mass planet abundance ~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. Object Class 3, already known onesPlanet evolution and atmospheres discovered by RV, 8-m direct imaging (SPHERE, GPI) or astrometric methods (GAIA, PRIMA) From ESO/ESA WG report GAIA discovery space SPHERE discovery space 7

8. Contrast requirements summary

9. Concept 9

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

11. 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) Advanced RTC algorithms studied in parallel to EPICS phase-A Simulation by Visa Korkiakoski 11 AO + coro

12. 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 Aller-Carpentier, proc. AO4ELT

13.  700K object next to K0 star HOT: XAO with APL coronagraph Martinez et al., submitted to A&AL • Good agreement with SPHERE simulations • Additional gain by quasi-static speckle calibration (SDI, ADI)

14. Residual PSF calibration From systematic PSF residuals (10-6-10-7) to 10-8-10-9 Spectral Deconvolution (Sparks&Ford, Thatte et al.), Trade-off: spectral bandwidth vs inner working angle, IFS (baseline Y-H) Polarimetric differential imaging for smallest separation, needs planet “feature” (e.g. CH4 band, or polarization) EPOL (600-900 nm) Coherence based methods (speckles interfere with Airy Pattern, a planet does not)  Self-Coherent camera (Baudoz et al, Proc. AO4ELT) Angular Differential Imaging (ADI)  All

15. Example: Spectral Deconvolution 15

16. Speckle chromaticity and Fresnel SD needs “smooth” speckle spectrum -> near-pupil optics 20 nm rms at 10x Talbot 20 nm rms in pupil plane

17. Apodizer End-2-end analysis Apodizer only leads to improved final contrast APLC

18. Baseline Concept All optics near the pupil planeminimize amplitude errors and speckle irregular chromaticity

19. Detection limits, incl. photon noise G2 star, 20 pc, 10h G2 star, 3pc, 10h Ph noise w/o spider data removal Flat Field 10-4 Systematics Systematics Ph noise with spider data removal

20. Detection rates, MC simulation 20

21. Predicted Science Output MC simulations • planet population with orbit and mass distribution from Mordasini et al. (2009) • 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

22. Detection rates, nearby+young stars Contrast requirements Simulations by M. Bonavita

23. Predicted EPICS output 23

24. 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)