1. High-precision eclipse photometry for CoRoT planets CoRoT symposium 2009 Feb 2 - 5, Paris M. Gillon (Geneva - Liege) & A. Lanotte, T. Barman, B.-O. Demory, A. Triaud, D. Queloz, F. Bouchy, H. Deeg, M. Deleuil, P. Magain, C. Moutou, J. Schneider, B. Tingley

2. Eclipse photometry for CoRoT planets I. Transit photometry Why bother? CoRoT photometry is great! CoRoT-Exo-1 (Barge et al. 2008) CoRoT-Exo-2 (Alonso et al. 2008)

3. Eclipse photometry for CoRoT planets I. Transit photometry Limb-darkening + spots effects are large at CoRoT effective wavelength

4. Eclipse photometry for CoRoT planets I. Transit photometry Limb-darkening + spots effects are large at CoRoT effective wavelength Independent determination of system parameters: check for folding effects, depth differences, dilution of the signal, etc…

5. Eclipse photometry for CoRoT planets I. Transit photometry Limb-darkening + spots effects are large at CoRoT effective wavelength Independent determination of system parameters: check for folding effects, depth differences, dilution of the signal, etc… Improvement of the ephemeris due to the longer baseline (eccentricity)

6. Eclipse photometry for CoRoT planets I. Transit photometry Limb-darkening + spots effects are large at CoRoT effective wavelength Independent determination of system parameters: check for folding effects, depth differences, dilution of the signal, etc… Improvement of the ephemeris due to the longer baseline (eccentricity) Transit timing and duration variations

7. Eclipse photometry for CoRoT planets I. Transit photometry Limb-darkening + spots effects are large at CoRoT effective wavelength Independent determination of system parameters: check for folding effects, depth differences, dilution of the signal, etc… Improvement of the ephemeris due to the longer baseline (eccentricity) Transit timing and duration variations High cadence sub-mmag transit photometry in a much redder bandpass than CoRoT’s

8. Eclipse Photometry for CoRoT planets I. Transit photometry see also Johnson et al. (2008) & Winn et al. (2009) Gillon et al. (2008)  = 550 ppm for dT = 54s, 1 transit vs  = 300 ppm for dT = 130s (Exo-1, 34 transits)

9. Eclipse photometry for CoRoT planets II. Occultation photometry Measurement of the planetary thermal emission at different wavelengths Broadband spectrum of exoplanets: atmospheric composition and physics (e.g. T inversion, albedo, heat distribution…)

10. Eclipse photometry for CoRoT planets II. Occultation photometry Measurement of the planetary thermal emission at different wavelengths Broadband spectra of exoplanets: atmospheric composition and physics (e.g. T inversion, albedo, heat distribution…) Occultation timing and duration constrain the orbital eccentricity Tidal evolution Tidal heating

11. Eclipse photometry for CoRoT planets II. Occultation photometry Measurement of the planetary thermal emission at different wavelengths Broadband spectra of exoplanets: atmospheric composition and physics (e.g. T inversion, albedo, heat distribution…) Occultation timing and duration constrain the orbital eccentricity Tidal evolution Tidal heating Near-IR mmag to sub-mmag photometry

12. Spitzer Space Telescope (NASA) Ground-based measurements! Eclipse photometry for CoRoT planets II. Occultation photometry TrES-3, 2.2  m De Mooij & Snellen (2009) OGLE-TR-56, 0.9  m Sing & Lopez-Morales (2009)

13. 1 transit observed with VLT/FORS in R filter 1 occultation observed with VLT/HAWK-I in the narrow band filter ND2090 ( =2.09  m, width = 20 nm) Global analysis with CoRoT photometry (36 transits) + SOPHIE RVs using a MCMC algorithm CoRoT-Exo-1

14. I. VLT/FORS R-band transit Fixing the ephemeris: transit too late 2  increase of the period -> OK

15. CoRoT-Exo-1 II. VLT/HAWK-I 2.1  m occultation Firm ground-based detection of the thermal emission Occultation is also too late

16. CoRoT-Exo-1 Global analysis Fixing T 0 and letting P vary Good transit fit but occultation seems still to be “too late”

17. CoRoT-Exo-1 Global analysis Letting e free: e = 0.017 +- 0.07 dF = 0.265 +- 0.035 % -> T b = 2460 K …preliminary result …

18. CoRoT-Exo-2 1 partial transit observed with VLT/FORS in z- band filter 1 occultation observed with Spitzer Space Telescope at 4.5 and 8  m Global analysis with CoRoT photometry + HARPS/CORALIE/SOPHIE RVs using a MCMC algorithm

19. CoRoT-Exo-2 I. VLT/FORS z-band transit Nice photometry, but incomplete transit will not provide an independent determination of the system parameters

20. CoRoT-Exo-2 II. Spitzer occultations 4.5  m8  m PSF blended with nearby fainter star in Spitzer images Deconvolution photometry ongoing See also poster Alonso et al.

21. Thank you for your attention !