eric pantin, jean schneider, a. boccaletti, p. baudoz, r. galicher, r. gratton, d. stam et al....

Eric Pantin,

Jean Schneider, A. Boccaletti, P. Baudoz, R. Galicher, R. Gratton,

D. Stam et al.

Polarimetry and spectral imaging

of mature Jupiter and super-Earth

with SEE-COAST

SEE-COAST UCF Orlando 2

Direct

imaging

Complementarity of techniques

SPECTRA & POLARIZATION

DATA

Transi

t


Space-based

Ground-based

1995 2000 2011 2017-20202010 >2025-30

We are here

Ground/space complementarity


Space-based

Ground-based

1995 2000 2011 2017-2020 >2025-30

8m + OA

VLT, Keck,

Gemini

4m + OA

Silla, CFH

We are here

2010


HST


Space-based

Ground-based

1995 2000 2011 2017-2020 >2025-30

We are here

2010

8m + XAO

SPHERE / GPI / HICIAO

NIR : EGPs young/massive/nearby


8m + OA

VLT, Keck,

Gemini

4m + OA

Silla, CFH

HST


Space-based

Ground-based

1995 2000 2011 2017-2020 >2025-30

We are here

2010


8m + OA

VLT, Keck,

Gemini

4m + OA

Silla, CFH

HST

30/42m + XAO

EPICS, METIS etc with ELTs

NIR : EGPs intermediate

Old + Super-Earth ?

8m + XAO




Space-based

Ground-based

1995 2000 2011 2017-2020

JWST

NIR + MIR:

Old EGPs>2025-30

We are here

2010

SPICA MIR:

Old EGPs


8m + OA

VLT, Keck,

Gemini

4m + OA

Silla, CFH

HST

30/42m + XAO

EPICS, METIS etc with ELTs


Old + Super-Earth ?

8m + XAO




Space-based

Ground-based

1995 2000 2011 2017-2020

Darwin/TPF-I

MIR: Earth

TPF-C

Vis: Earth

>2025-30

We are here

?

?

2010

JWST

NIR + MIR:

Old EGPs

SPICA MIR:

Old EGPs


8m + OA

VLT, Keck,

Gemini

4m + OA

Silla, CFH

HST

30/42m + XAO

EPICS, METIS, etc with ELTs


Old + Super-Earth ?

8m + XAO




Space-based

Ground-based

1995 2000 2011 2017-2020 >2025-30

Visible light

Old giants & super-Earths

We are here

?

?

2010

JWST

NIR + MIR:

Old EGPs

SPICA MIR:

Old EGPs Darwin/TPF-I

MIR: Earth

TPF-C

Vis: Earth

?

?Ground/space complementarity

8m + OA

VLT, Keck,

Gemini

4m + OA

Silla, CFH

HST

30/42m + XAO

EPICS, METIS, etc with ELTs


Old + Super-Earth ?

8m + XAO



Opportunity for space

projects


Space-based

Ground-based

1995 2000 2011 2017-2020 >2025-30

We are here

?

?

2010

JWST

NIR + MIR:

Old EGPs

SPICA MIR:

Old EGPs Darwin/TPF-I

MIR: Earth

TPF-C

Vis: Earth

?

?

SEE COAST Vis/NIR

Old Jupiter + Super Earth


8m + OA

VLT, Keck,

Gemini

4m + OA

Silla, CFH

HST

30/42m + XAO

EPICS, PFI, etc with ELTs


Old + Super-Earth ?

8m + XAO




What SEE-COAST will characterize :

What's expected :

Exo-zodiacal and debris disk

Mature Jupiter (>1 Gyr)

And unexpected objects !Stay open-minded (cf. hot Jupiter in 1995)

Brighter

Atmosphere, climate

Variations, habitability

Super

Earth

Around nearby star

-


Spectroscopy : chemical composition

Giant planets

Solid planets


Polarimetry : physical informationsJupiter-like planet - Stam et al. 2005

Spectrum

Polarization

Earth-like planet - Stam et al. 2008

cloud

vegetation

oceanA=0

A=1

SEE-COAST UCF Orlando

- 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


How many detections ?



1e-9

1e-10



1e-9

1e-10

Requirements : 10-10 contrast Small inner working angles


Hyperbolic secondary mirror 4,85m long

Parabolic primary mirror

Two folding

mirrors

Focal plane Submitted in 2007 to

ESA Cosmic Vision

SEE-COAST proposed to ESA Cosmic VisionParameter Value

Entrance pupil diameter D > 1.5m

Angular resolution 70 mas @ 0.6 m

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


1) Coronagraphy2) Wavefront control (a few nm rms from science image)

3) Polarization+Spectral Differential imaging

SEE-COAST : optical concept

1) visible light channel (0.4-0.85 m): 2 polarimetric arms

2) Near-IR channel (0.85-1.25 m): no polarimetry


Main component I: Achromatic Coronagraph

Laboratory "planet"

Contrast : 6.7 10- 9

at 4.5/D= 20%

Visible lightBaudoz et al. 2007, 08

Multi-stage four quadrant

phase mask coronagraph


Main component II: Wavefront correction

Speckle nulling

in a limited FOV

with a DM (JPL, Trauger

& Traub, 07)

2 stages WFS: 1st stage : Classical WFS+DM (~1 nm rms residuals) 2nd stage : Phase correction in coronagraphic image : wavefront error

reduced by 100, spurious speckles by a factor 10 000 (speckles nulling).

2 DMs concept is preferred (and envisioned)


Main component III :

Integral Field Spectrometer (R=40-80)

Field position

Wavelength


Main component IV :

Reject efficiently spurious star speckles

1) differential polarimetry

Field position

Wavelength

2) spectral deconvolution (aberrations scale with )

Wavelength

3) Self-coherent method (Baudoz, 07)


SummarySEE 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)

eric pantin, jean schneider, a. boccaletti, p. baudoz, r. galicher, r. gratton, d. stam et al....

Documents

dsee coast

raphal galicherhow

toesa cosmic visionseecoast

hot jupiter

polarimetrymain component

planet stam

phase correction

wavefront error