pierre baudoz (paris observatory) a. boccaletti, d. mawet, j. schneider, g. tinetti, r. galicher, c....

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

SPICA MIR:Old EGPs

Direct Imaging Programs Overview

Space-based

Ground-based

1995 2000 2011 2017-20202008

SEE COASTVis/NIR: Old Jupiter+ Super Earth

Darwin/TPF-I MIR: Earth

TPF-CVis: Earth

JWSTNIR + MIR: Old EGPs

8m + XAOSPHERE / GPI / HiCIAONIR : EGPs young/massive/nearby

30/42m + XAOEPICS/ELTsNIR : EGPs intermediate Old + Super-Earth ?

>2025-30

HSTOpportunity for Space projects

In the Visible

mature giants & Super-Earths

8m + OAVLT, Keck,Gemini, Subaru

4m + OASilla, CFH

We already have targets !!!

From radial velocity surveys : From direct imaging :

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 ?

Explore the Diversity with SEE COAST

- Spectra => Chemical composition

Burrows, Sudarsky

- Rayleigh scatterring => pressure, surf. reflectivity

• Spectroscopy

Explore the Diversity

• Spectroscopy• Polarimetry- Polarization=> Clouds / albedo

Jupiter-like planet - Stam et al. 2005Earth-like planet - Stam et al. 2008

cloud

vegetation

oceanA=0

A=1

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

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

A proposal to Cosmic Vision …

✔Submitted in 2007 to ESA Cosmic Vision

Parameter Value

Entrance pupil diameter D > 1.5m

Angular resolution 70 mas @ 0.6 m

Spectral Range 0.4 to 1.2 m

Spectral Resolution R>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

Coronagraphy: Multi 4QPM

Baudoz et al. 2007, 08

laboratory planetContrast :6.7 10-9bandwidth 20%

Multi 4QPM : Meudon

N phase masks in series => Improves bandwidth as ^NPupil

Telescope

FQPM # 1

FQPM # 3FQPM # 2

Wavefront correction : Coherence

Speckle nullingin a limited FOV with a DM (JPL)

Summary

SEE COAST requires : • High contrast : ≈ 10-10 AND small 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)