1 / 13

Spectroscopic follow-up of transiting exoplanet surveys FLAMES follow-up of OGLE III

Spectroscopic follow-up of transiting exoplanet surveys FLAMES follow-up of OGLE III. Frédéric Pont (Geneva) Francois Bouchy (Mar seille), Claudio Melo (ESO), Nuno Santos (Lisbon), Didier Queloz, Stephane Udry, Michel Mayor (Geneva). 10. 7 known transiting exoplanets. HD 209458 TrES-1

nelia
Download Presentation

Spectroscopic follow-up of transiting exoplanet surveys FLAMES follow-up of OGLE III

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. Spectroscopic follow-up of transiting exoplanet surveysFLAMES follow-up of OGLE III Frédéric Pont (Geneva) Francois Bouchy (Marseille), Claudio Melo (ESO), Nuno Santos (Lisbon), Didier Queloz, Stephane Udry, Michel Mayor (Geneva)

  2. 10 7 known transiting exoplanets HD 209458 TrES-1 OGLE-TR-10 OGLE-TR-56 OGLE-TR-111 OGLE-TR-113 OGLE-TR-132 mass-radius relation for hot gas giants

  3. The OGLE-III program Ground-based photometric survey for planetary transits ~100’000 targets / square degree 177 transiting candidates in the Galactic disc Rc RJupiter Pc : 0.8 - 8 days V : 15-18 mag  : 5-15 mmag spectroscopic follow-up requires large telescope and <100 m/s accuracy Udalski et al. 2002abc, 2003, 2005, Acta Astr.

  4. FLAMES+UVES facilities on the VLT • Field of view 25 arcmin • Multi-fiber link • to UVES spectrograph • (7 targets + 1 Tho) • R ~ 45’000  = 480 – 680 nm • 45 mn on mv=17 • S/N ~ 8  ~30 m/s (The fiber eliminates ~100m/s centering uncertainty in slit)

  5. Doppler follow-up with UVES+FLAMES 2 x 4 nights on VLT 60 best targets followed using multi-fiber and strategy of real-time fiber reallocation

  6. 5 transiting hot Jupiters from the OGLE survey OGLE-TR-56 P=1.2 days Konacki et al. 2003 OGLE-TR-10 P=3.1 days Bouchy et al. 2005, Konacki et al. 2005 OGLE-TR-111 P=4.0 days Pont et al. 2004 OGLE-TR-113 P=1.43 days Bouchy et al. 2004, Konacki et al. 2004 OGLE-TR-132 P=1.69 days Bouchy et al. 2004, Moutou et al. 2004

  7. Stellar transits and eclipses Various configurations of eclipsing binaries can mimic a planetary transit signal grazing eclipses small M-dwarf transits triple/quadruple systems Light curves (Udalski et al. 2002) Velocity curves (Bouchy et al. 2005, Pont et al. 2005)

  8. M dwarfs Transiting hot Jupiters Planet-sized brown-dwarf edge The mass-radius relation from stars to planets

  9. HST SMALL TELESCOPES OGLE Spectroscopic follow-up of transit surveys

  10. The example of OGLE-TR-122b A planet-sized M dwarf M = 96 MJR= 1.2 RJP=7.4 daysgravitational modulation nnn mmaganti-transit photometric signalundistinguishable fromplanetary transit !

  11. Conclusions Spectroscopic follow-up is essential to determine the nature of transiting candidates Possible up to V=18 with FLAMES on the VLT Most candidates are eclipsing binaries (numerous confusion scenarios) Medium-deep surveys offer optimal combination of target density and spectroscopic capabilities

  12. OGLE-TR-113b 0.5 MJ HD209458b 0.5 MJ Saturn 0.3 MJ OGLE-TR-123b 70 MJ OGLE-TR-122b 90 MJ

  13. OGLE-TR-113 0.5 MJ HD209458b 0.5 MJ Saturn 0.3 MJ OGLE-TR-123b 70 MJ OGLE-TR-122b 90 MJ

More Related