1. Pierre BAUDOZ (Paris Observatory) A. Boccaletti, D. Mawet, J. Schneider, G. Tinetti, R. Galicher, C. Cavarroc J. Hough, P. Doel, D. Pinfield, C.-U. Keller, J.-L. Beuzit, S. Udry, M. Ferrari, E. Martin, F. Ménard, E. Sein, & SEE COAST Team … ULg / CSL / LESIA / LUTH / LUAN / ETH-Zurich / IAP / Obs. Geneva / U. Bern / UCL / ROE / U. Hertfords. / MSSL / SRON / Astron / U. Utrecht / LAOG / ONERA / DLR / U. Vienna / U. Nantes / U. Torino / Astrium Probing the Extrasolar Planet Diversity with SEE COAST

2. SPICA MIR: Old EGPs Direct Imaging Programs Overview Space-based Ground-based 1995200020112017-20202008 SEE COAST Vis/NIR: Old Jupiter + Super Earth Darwin/TPF-I MIR: Earth TPF-C Vis: Earth JWST NIR + MIR: Old EGPs 8m + XAO SPHERE / GPI / HiCIAO NIR : EGPs young/massive/ne arby 30/42m + XAO EPICS/ELTs NIR : EGPs intermediate Old + Super-Earth ? >2025-30 HST Opportunity for Space projects In the Visible mature giants & Super-Earths 8m + OA VLT, Keck, Gemini, Subaru 4m + OA Silla, CFH

3. We already have targets !!! From radial velocity surveys :From direct imaging :

4. More targets to come We can anticipate many RV planets at longer periods (giants and tellurics) A few accessible from SPHERE/GPI/HiCIAO (1. - 2.3 m) and JWST (2.5 - 28 m) Motivation for exploring a different spectral range (in the visible) angular resolution AND contrast are required: A small telescope in space can be optimized for exo-planetology "Super Earth" as a sweet spot : brighter, earth-like notions apply (atmosphere, climate, variations, habitability, …) What sort of astrophysics on these planets ?

5. Explore the Diversity with SEE COAST - Spectra => Chemical composition Burrows, Sudarsky - Rayleigh scatterring => pressure, surf. reflectivity Spectroscopy

6. Explore the Diversity Spectroscopy Polarimetry - Polarization => Clouds / albedo Jupiter-like planet - Stam et al. 2005 Earth-like planet - Stam et al. 2008 cloud vegetation ocean A=0 A=1

7. Explore the Diversity - Spectral time variation => variation of temperature => surface properties 0.45 m 0.75 m - Polarimetric time variation => surface properties Cloud free Earth from 0.65 to 0.9 m 50° Phase angle 130° 90° Spectroscopy Polarimetry Variability

8. Which targets ? (contrast + IWA requirements) short wavelengths are optimal longer wavelengths require small IWA coronagraph (2 /D) near IR (1 - 1.2 m) - self luminous planets - T > 800K 10 -10 contrast required

9. A proposal to Cosmic Vision … Submitted in 2007 to ESA Cosmic Vision Parameter Value Entrance pupil diameterD > 1.5m Angular resolution 70 mas @ 0.6 m Spectral Range 0.4 to 1.2 m Spectral ResolutionR>40 Contrast (after speckle subtraction) @ 2 /D < 10 -9 Contrast (after speckle subtraction) @ 4 /D < 10 -10 Orbit for 6 months visibility, high thermal stability L2 Lagrangian Hyperbolic secondary mirror 4,85 m long Parabolic primary mirror Two folding mirrors Focal plane

10. Coronagraphy: Multi 4QPM Baudoz et al. 2007, 08 laboratory planet Contrast :6.7 10 -9 bandwidth 20% Multi 4QPM : Meudon N phase masks in series => Improves bandwidth as ^N Pupil Telescope FQPM # 1 FQPM # 3 FQPM # 2

11. Wavefront correction : Coherence Speckle nulling in a limited FOV with a DM (JPL)

12. Summary SEE COAST requires : High contrast : 10 -10 ANDsmall IWA : 2 /D SEE COAST can get : low res spectra of mature giants < 20pc (< 8 - 10 AU) colors of a few mature Super Earths < 10pc (< 4 - 5 AU) possibly Earths around the nearest star ( Cen) low res spectra of self luminous planets (extension to near IR) SEE COAST is : Compatible with general astrophysics (pushing to UV, wide field ?) Compatible with transit spectroscopy – additional targets (unresolved planets) & complements IR transit characterization programs Next steps in the project : refine some science cases and simulations (statistical analysis) elaborate optical design with industrial partners (Astrium) + derive tolerances technological developments in coronagraphy and wavefront control get prepared for next COSMIC VISION proposal (2010)