TITRE
description
Transcript of TITRE
TITRESearch and Characterization of Extrasolar planets
in Antartica
François BouchyInstitut d’Astrophysique de Paris
Status : ~ 200 known extrasolar planets
Earth
Jup
Sat
10 transiting extrasolar planetsCharacterized by photometry and radial velocity
VHJ
10 transiting extrasolar planetsCharacterized by photometry and radial velocity
VHJ
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
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Lack of efficiency of photometric surveys
More than 200 planets per month were expected
Up to day a total of only 7 detections
1st main limitation : time coverage
Most abundant Hot Jupiters [3-4 d]
Tres-1 [3.03 d]OGLE-10b [3.10 d]
Xo-1 [3.94 d]OGLE-111b [4.02 d]
OGLE-56b [1.21 d]OGLE-113b [1.43 d]OGLE-132b [1.69 d]
Need of continuous coverage
60-day continuous coverage (Antarctica)
60-day nighttime coverage (OGLE)
Period [days]
2nd main limitation : systematic errors
HD209458OGLE-TR-10OGLE-TR-132
1%
Tres-1
Transit Depth
OGLE-113 2.9% Tres-1 2.3%Xo-1 2.0%OGLE-111 1.9%OGLE-10 1.9%OGLE-56 1.3 %OGLE-132 1.1 %
No transiting planet detected with a depth < 1.1%
mmag precision is possible from ground
OGLE-113 with SUSI/NTTOGLE-132 with FORS/VLT
HD149036
Gillon et al. submitted
Sato et al. (2005)
Moutou et al. (2004)
systematic errors due to the atmosphere are expected to be considerably reduced ….
Need of stable atmospheric conditions
… but not systematic errors due to the instrument !
- intra pixel response- Flat field stability - ….
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
Main Scientific goals of photometric survey for transiting planets
Detect and characterizetransiting Hot Neptunes
Sub mmag clearly required
Main Scientific goals of photometric survey for transiting planets
Detect and characterizetransiting big Earth in the habitable zone of M-K dwarfs
Several seasons on the same fields
Mass-radius relation from planets to BDs and to low mass stars
Galactic plane visible from Dome C during 3 month with secz < 2.
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
Secondary objectives of photometric survey :
- Stellar pulsation - Stellar activity- Eclipsing binaries - ….
Conclusions
• 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