1. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 1 Direct Imaging of Extrasolar Planets Overview of Ground & Space Programs Anthony Boccaletti : Obs. Paris-Meudon

2. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 2 Outline 1. A brief introduction to the high contrast imaging problematic 2. A brief review of projects (talks to follow) 4. « Where » do we need to direct our effort

3. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 3 No longer a dream ! 2M12075 M J 46 AU GQ Lup17 M J 100 AU AB Pic14 M J 248 AU CHRX7312 M J 210 AU HN Peg16 M J 795 AU DH Tau12 M J 330 AU RSX 16098 M J 330 AU Detection was made possible because : - small mass ratios (contrast is lower) - young ages (planet is brighter) - large physical / angular separations

4. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 4 A few more last week … Fomalhaut< 3 M J 120 AU HR8799 b5 M J 46 AU HR8799 c12 M J 330 AU HR8799 d8 M J 330 AU

5. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 5 Problematic Planets are faint and close …. 10 9 = 1 milliard 10 6 = 1 million Reflected lightThermal emission STOP !!!! … What about diffraction ???

6. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 6 Problematic Stellar images are not point-like …

7. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 7 Solutions to reduce diffraction Yes but … the Sun is an extended source Stars are point sources => diffraction is much stronger We need more performant stellar coronagraphs … to attenuate stars We need BIG telescopes … We need to attenuate the star

8. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 8 In Theory … si Plan A: Plan B: Plan C:Plan D:

9. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 9 We are working on it..

10. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 10 Problematic (again) Instruments are not perfect …. unfortunately Many defects : - atmospheric turbulence for ground based telescopes - static (more or less) optical aberrations - variation of transmission - alignment - chromaticity - … => Limits the performance of coronagraphs

11. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 11 Solutions to reject speckles Wavefront Correction : at focal plane - speckles minimization - Self Coherent Camera Wavefront Calibration : Differential imaging - spectral (SDI, SD) - angular (ADI) - polarimetric (PDI) JPL Testbed SCC simulation SDI, Gemini ADI, Gemini SD, VLT

12. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 12 Planned Projects

13. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 13 Planet Finders on 8m telescopes (2011) European Consoritum, VLT - Dual band NIR camera (YJHK) - NIR IFS (YJH) - Dual Polarisation VIS camera eXtreme AO + coronagraphy + differential imaging HiCIAO Japan, Subaru - Dual band NIR camera - Dual polarisation NIR camera HiCIAO + (in dev., 2010) - Focal Plane WF - coronagraph improvement - NIR IFS US, Gemini South - NIR IFS (YJH) Focal Plane Looking at Giant Planets in : - young associations of stars (10 Myrs <100pc) - stars with known planets (RV surveys) - stars of intermediate age (0.1-1 Gyr) - very nearby bright stars

14. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 14 MIRI Europe + US consortium 5 - 28  m imager + IFU MIRI imager has 4 coronagraphs 4QPM in 3 filters (10.6, 11.4, 15.5  m) => self luminous mature giants T > 300-400K (5 - 10AU, 10pc, 5Gyr) Expected contrast : 10 4 - 10 5 - photometry (R=20) James Webb Space Telescope (2014) =11.40  m CSA responsabilty 1 - 5  m tunable filter with coronagraphic capabilities (Spectral Deconvolution) - spectra (R=100) US instrument 0.6 - 5  m imager NIRCAM has 5 coronagraphs Optimized for several filters (F200, F480, …) Good performance at 4.8  m At 2.2  m mature giants are too faint. Expected contrast : 10 5 - 10 6 - photometry (R=10-20) NIRCAM MIRI FGS - TFI & SPICA

15. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 15 Extremely Large Telescopes (2020) objectives : - mature giants - irradiated planets heritage of VIZIR & MIRI /D = 50mas Photometry + spectra heritage of SPHERE / GPI / HiCIAO /D = 10mas - Photometry + spectra objectives : - young giants - mature giants, spectral characterization - Super Earth : detection + 1st order charac.

16. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 16 Future projects … in space Extend spectroscopic characterization towards ; - shorter wavelengths (<1  m) - lower masses (Super Earths, Earths) - shorter separations (< 1 AU) - older objects (1 - 5 Gyr) - more distant stars (> 100 pc) - …

17. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 17 Single spacecraft (later than 2020) Small Telescopes : 1.5 - 2m - optical quality - efficient coronagraph - focal plane WFS and correction - differential imaging 3 studies in the US : - PECO - ACCESS=> Probe Class (Decadal Survey) - EPIC - SEE-COAST => CV proposal - spectra : 0.4 - 1.0  m (R>50) - polarimetry : 0.4 - 0.85  m objectives : - explore diversity of planets - mature giants in the visible - Super Earths - target list : HARPS, ESPRESSO, GAIA, COROT, KEPLER, …

18. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 18 Two spacecrafts: towards tellurics External OcculterFresnel imaging lens Occulter : 50 m Telescope : 4 m Separation : 80 000 km Optimize for Vis. and UV : 0.4 -1.1  m Chromatic High throughput Occulter : 50 m Telescope : 4 m Separation : 80 000 km Optimize for Vis. and UV : 0.4 -1.1  m Chromatic High throughput Lens : 3.6 m Telescope : 68 cm Separation : 2.5 - 20 km Optimize for Vis. and UV : 0.1 -1  m Chromatic Low throughput Lens : 3.6 m Telescope : 68 cm Separation : 2.5 - 20 km Optimize for Vis. and UV : 0.1 -1  m Chromatic Low throughput

19. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 19 Timeline SPACE GROUND Vis / MIR - old EGPs - Super Earths - Earths JWST NIR + MIR old / close EGPs 8m + XAO SPHERE / GPI / HiCIAO NIR young / massive / close EGPs 30 - 40 m + XAO EPICS / PFI NIR + MIR old EGPs / Super Earth 8m + AO VLT, Keck, Gemini NIR 4m + AO Silla, CFH NIR Room for missions ! 19952000 20112017-2020 20072014 HST Vis

20. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 20 Mass vs. Wavelength coverage Space telescopes Occulters Space Interferometry 10 M J 1 M J 10 M  1 M 

21. Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008 21 A few conclusions … 1.high contrast imaging allows to study molecules in the atmosphere of a wide variety of objects 2.see the talks of this afternoon for details 3.most instruments focused on EGPs in the NIR & MIR 4.There is a gap between EGPs and Earth-like planets spectrocopy 5.What’s next (short timescale) : - spectroscopy of EGPs in the visible - Super Earths are numerous - MIR : space interferometry more promising (see talk this afternoon)