TITRE
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Transcript of TITRE
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TITRESearch and Characterization of Extrasolar planets
in Antartica
François BouchyInstitut d’Astrophysique de Paris
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Status : ~ 200 known extrasolar planets
Earth
Jup
Sat
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10 transiting extrasolar planetsCharacterized by photometry and radial velocity
VHJ
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10 transiting extrasolar planetsCharacterized by photometry and radial velocity
VHJ
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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
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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]
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Need of continuous coverage
60-day continuous coverage (Antarctica)
60-day nighttime coverage (OGLE)
Period [days]
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2nd main limitation : systematic errors
HD209458OGLE-TR-10OGLE-TR-132
1%
Tres-1
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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%
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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)
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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 - ….
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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
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Main Scientific goals of photometric survey for transiting planets
Detect and characterizetransiting Hot Neptunes
Sub mmag clearly required
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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
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Mass-radius relation from planets to BDs and to low mass stars
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Galactic plane visible from Dome C during 3 month with secz < 2.
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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
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Secondary objectives of photometric survey :
- Stellar pulsation - Stellar activity- Eclipsing binaries - ….
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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