Molecules

Molecules

in the tmospheresof extrasolar planets

Observatoire de Paris, Salle Cassini, November 19-21, 2008

SPEEDY POSTERS SPEEDY POSTERS

SPEEDY POSTERS SPEEDY POSTERS

GONE IN 60 SECONDS !GONE IN 60 SECONDS !

Ground-based detection of the secondary eclipse of TrES-3bErnst de Mooij & Ignas Snellen, Leiden Observatory

ΔF = -0.234 ± 0.028%Δφ = -0.0041 ± 0.0018

Observations with the William Herschel Telescope

Exoplanet spectroscopy: the Hubble casePieter Deroo

M. Swain, G. Vasisht, A. Tanner, P. Chin, G. Tinetti, J. Bouwman, D. Deming, Y. Yung

Very high dynamic range imaging up to 106 at visible wavelengths

A new idea for aperture masking: FIRST (Fibered Imager foR Single Telescope)

Redundant Array + Corrugated Wavefront

Non-Redundant Array + Spatially Filtered Wavefront

Single-mode fibers

Lenslet array

FIRST project: Planet detection from the ground at visible to near-infrared wavelengths without using Adaptive Optics

T. Kotani

Reconstructed Image

CCD Imaging

Pupil remapping + single-mode fiber

Lab Demonstration

Exoplanet research with Exoplanet research with SAFARISAFARI::

A far- A far-IR IR imaging spectrometer for imaging spectrometer for SPICASPICAJavier R. GoicoecheaJavier R. Goicoechea (UCM/CSIC, Madrid, Spain) Kate IsaakKate Isaak (Cardiff University, U.K.)Bruce SwinyardBruce Swinyard (Rutherford Appleton Laboratory, U.K.)

On behalf of the SAFARI consortium

JAXA-led SPICA Mission:JAXA-led SPICA Mission: mid- and far-mid- and far-IRIR

cooled (<5 K) space telescope (D~3.5m)cooled (<5 K) space telescope (D~3.5m)

SAFARISAFARI instrument: instrument: far-far-IRIR imaging-FTSimaging-FTS

• Wavelength coverage of Wavelength coverage of ~33-210~33-210mm

• Field of view of Field of view of ~~2’ x 2’2’ x 2’

• Spectroscopy Spectroscopy (R(R~~2,000)2,000) & photometry & photometry (R~3)(R~3)

Science questionsScience questions in the field of exoplanetsexoplanets and planet formationplanet formation with SAFARI:SAFARI:

• Stellar far-Stellar far-IRIR photometric excessesphotometric excesses (disks!).(disks!).

• Protoplanetary disks: from gas toProtoplanetary disks: from gas to “snow lines”“snow lines”..

• Primary and secondaryPrimary and secondary transits transits in the far-in the far-IRIR..

• Searching forSearching for spectral signaturesspectral signatures of transiting of transiting exoplanets (water vapor, HD, biomarkers…).exoplanets (water vapor, HD, biomarkers…).

What could be observed in the case of Super-Ios and Hyper-Ios?

Danielle Briot & Jean Schneider

We study the case of a Earth, or a Super-Earth with a volcanic activity as strong as Io’s. We call such an object a Super-Io and a Hyper-Io in the case of a

Super-Earth.- In case of a transit, sulphur dioxid could be observed in the

atmosphere- These objects are very good candidates for secondary transits

observations, specially at 3.5 m, and the hot spots corresponding to volcanoes could be detected in the first part and the last part of the secondary transit.

- These objects could be easily observed by imaging in the infrared, specially in a case of a cool star.

ExoFit A Bayesian multi-planet fitting software for planet hunters

Sreekumar Thaithara Balan1 & Ofer Lahav2

1. Cavendish Labs, University of Cambridge, CB3 0HE,UK email: [email protected]. University College London, WC1E 6BT, UK, email: [email protected]

Best fit Keplerian orbital solution for HD 159868 Posterior distribution of orbital parameters and other useful astronomical quantities for HD 159868

The young, tight and low mass binary TWA22AB: a new calibrator for evolutionary models ?

1 Laboratoire d’Astrophysique - Observatoire de Grenoble (LAOG), FRANCE2 European Southern Observatory (ESO), Chile

3 Department of Physics and Astronomy, University of Georgia, USA

E-mail : [email protected]

M. Bonnefoy1, G. Chauvin1, C. Dumas2, A-M. Lagrange1, H. Beust1, M. Desort1, J-L. Beuzit1 and I. Song3

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Paper submitted (Bonnefoy et al. 2008)

Aim: calibrating evolutionary models at young ages and at the substellar boundary.

Observations of the young low mass binary TWA22 AB

with SINFONI and NACO

Physical parameters (Dynamical mass, effective

temperatures, gravities, luminosity, distance, age)

Comparison to evolutionary models predictions

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