1. Search and Characterization
TITRE
Search and Characterization
of Extrasolar planets
in Antartica
François Bouchy
Institut d’Astrophysique de Paris

2. Status : ~ 200 known extrasolar planets
Jup
Sat
Earth

3. 10 transiting extrasolar planets
Characterized by photometry and radial velocity
VHJ

4. 10 transiting extrasolar planets
Characterized by photometry and radial velocity
VHJ

5. Photometry + Radial Velocity + Spectroscopy
Fully complementary methods
a, P, e, T0, b, 
mp, rp, , mcore , T, evap. , …
R*, M*, [Fe/H], vsini, R’HK , …
Constraints for processes of formation and evolution
Constraints for composition and internal structure

6. Lack of efficiency of photometric surveys
More than 200 planets per month were expected
Up to day a total of only 7 detections

7. 1st main limitation : time coverage
OGLE-56b [1.21 d]
OGLE-113b [1.43 d]
OGLE-132b [1.69 d]
Tres [3.03 d]
OGLE-10b [3.10 d]
Xo [3.94 d]
OGLE-111b [4.02 d]
Most abundant Hot Jupiters
[3-4 d]

8. Need of continuous coverage
60-day continuous coverage (Antarctica)
60-day nighttime coverage (OGLE)
Period [days]

9. 2nd main limitation : systematic errors
HD209458
OGLE-TR-10
OGLE-TR-132
Tres-1 1%

10. No transiting planet detected with a depth < 1.1%
Transit Depth
OGLE %
Tres %
Xo %
OGLE %
OGLE %
OGLE %
OGLE %

11. mmag precision is possible from ground
HD149036
Sato et al. (2005)
OGLE-132 with FORS/VLT
OGLE-113 with SUSI/NTT
Gillon et al. submitted
Moutou et al. (2004)

12. Need of stable atmospheric conditions
systematic errors due to the atmosphere
are expected to be considerably reduced ….
… but not systematic errors due to the instrument !
- intra pixel response
- Flat field stability
- ….

13. Main Scientific goals of photometric survey for transiting planets
Increase the number of
transiting Hot Jupiters
especially around bright stars
for complementary and further
observations

14. Main Scientific goals of photometric survey for transiting planets
Detect and characterize
transiting Hot Neptunes
Sub mmag clearly required

15. Main Scientific goals of photometric survey for transiting planets
Detect and characterize
transiting big Earth in the
habitable zone of M-K dwarfs
Several seasons on the same fields

16. Mass-radius relation from planets
to BDs and to low mass stars

17. Galactic plane visible
from Dome C during 3 month
with secz < 2.

18. Doppler follow is required
- to discriminate confusing case
- to assess the planetary nature of the transit
- to determine the mass of the planet
ESO Facilities for South hemisphere already used for follow-up
(GIRAFFE / FLAMES-UVES / HARPS)
But limited to mv < 15.5

19. Secondary objectives of photometric survey :
Stellar pulsation
Stellar activity
Eclipsing binaries ….

20. Conclusions Transit survey in Dome C + Doppler follow-up
Continuous time coverage is crucial to exoplanet transit survey.
Better photometric conditions also allow to reach the planetary transit realm.
Transit survey in Dome C + Doppler follow-up
 huge contribution to the knowledge of exoplanets