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OHP2015: Twenty years of giant exoplanets The physical properties of giant transiting exoplanets within 400 days Collaborators: I. Boisse, F. Bouchy, G. Bruno, B. Courcol, M. Deleuil, O. Demangeon, C. Moutou, A. Rajpurohit (LAM) V.

  1. OHP2015: Twenty years of giant exoplanets The physical properties of giant transiting exoplanets within 400 days Collaborators: • I. Boisse, F. Bouchy, G. Bruno, B. Courcol, M. Deleuil, 
 O. Demangeon, C. Moutou, A. Rajpurohit (LAM) • V. Adibekyan, S. Barros, N. Santos, M. Tsantaki (IA-Porto) • L. Amard, R. Díaz, J. Rey (obs. Geneva) • G. Hébrard, G. Montagnier (IAP / OHP) • T. Guillot, M. Havel (OCA) Alexandre Santerne • J.-M. Almenara (IPAG) • A. Bonomo (INAF - Torino) Marie Curie Fellow Instituto de Astrofísica e Ciências do Espaço 
 Universidade do Porto Porto, Portugal alexandre.santerne@astro.up.pt 1

  2. 5 years ago… during the OHP2010 colloquium This is Kepler-9 c ! 2

  3. 5 years ago… during the OHP2010 colloquium Minimum mass This is This is HD10180 h ! Kepler-9 c ! 2

  4. 5 years ago… during the OHP2010 colloquium Minimum mass This is This is HD10180 h ! Kepler-9 c ! 2

  5. The Kepler candidates sample (Q1 - Q17) All KOIs 10 6 16 10 5 15 Kepler magnitude [K p ] Transit depth [ppm] 10 4 14 13 10 3 12 10 2 11 Santerne et al. (submitted) 10 10 1 10 0 10 1 10 2 10 3 Orbital period [days] 3

  6. The Kepler candidates sample (Q1 - Q17) All KOIs 10 6 16 10 5 15 Kepler magnitude [K p ] Transit depth [ppm] 10 4 14 13 10 3 12 10 2 11 Santerne et al. (submitted) 10 10 1 10 0 10 1 10 2 10 3 Orbital period [days] Kp < 14.7, Per < 400d, 0.4% < Depth < 3% ➙ 129 KOIs / 125 stars 3

  7. The Kepler candidates sample (Q1 - Q17) Selected giant KOIs All KOIs 10 6 3 . 5 16 16 3 . 0 10 5 15 15 Kepler magnitude [K p ] Kepler magnitude [K p ] 2 . 5 Transit depth [ppm] Transit depth [ % ] 10 4 14 14 2 . 0 13 13 10 3 1 . 5 12 12 1 . 0 10 2 11 11 Santerne et al. (submitted) 0 . 5 10 10 10 1 0 . 0 10 0 10 1 10 2 10 3 10 0 10 1 10 2 Orbital period [days] Orbital period [days] Kp < 14.7, Per < 400d, 0.4% < Depth < 3% ➙ 129 KOIs / 125 stars 3

  8. The Kepler candidates sample (Q1 - Q17) Selected giant KOIs All KOIs 10 6 3 . 5 3 . 5 Planets Unknown 16 16 16 3 . 0 3 . 0 10 5 15 15 15 Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] 2 . 5 2 . 5 Transit depth [ppm] Transit depth [ % ] Transit depth [ % ] 10 4 14 14 14 2 . 0 2 . 0 13 13 13 10 3 1 . 5 1 . 5 12 12 12 1 . 0 1 . 0 10 2 11 11 11 Santerne et al. (submitted) 0 . 5 0 . 5 10 10 10 10 1 0 . 0 0 . 0 10 0 10 1 10 2 10 3 10 0 10 0 10 1 10 1 10 2 10 2 Orbital period [days] Orbital period [days] Orbital period [days] Kp < 14.7, Per < 400d, 0.4% < Depth < 3% ➙ 129 KOIs / 125 stars 3

  9. Planets: to be or not to be Transit light-curve 1 . 002 planet 1 . 000 0 . 998 Santerne et al. (2014) Relative flux 0 . 996 0 . 994 S0 S2 0 . 992 planet in S1 S3 O-C [ppt] binary 1 . 5 0 . 0 − 1 . 5 − 0 . 0015 − 0 . 0010 − 0 . 0005 0 . 0000 0 . 0005 0 . 0010 0 . 0015 Orbital phase planet in binary or Binary / BD Triple or BEB background transiting planet 4

  10. The Kepler spectroscopic FUp program • 1.93 m telescope + SOPHIE spectrograph, HERE ! • Large program started in July 2010. • Radial velocity precision down to 13 m/s on magnitude 14.5. Santerne et al. (submitted) • More than 1000 spectra obtained over ~370 nights in 6 years (equivalent to 120 nights). + ~15 nights on HARPS-N @ TNG 5

  11. Unveiling the candidates’ nature 3 . 5 Planets Unknown 16 3 . 0 15 Kepler magnitude [K p ] 2 . 5 Transit depth [ % ] 14 2 . 0 13 1 . 5 12 1 . 0 11 0 . 5 10 0 . 0 10 0 10 1 10 2 Orbital period [days] 6 Santerne et al. (submitted)

  12. Unveiling the candidates’ nature 3 . 5 3 . 5 Planets Planets Unknown Unknown 16 16 3 . 0 3 . 0 15 15 Kepler magnitude [K p ] Kepler magnitude [K p ] 2 . 5 2 . 5 Transit depth [ % ] Transit depth [ % ] 14 14 2 . 0 2 . 0 13 13 1 . 5 1 . 5 12 12 1 . 0 1 . 0 11 11 0 . 5 0 . 5 10 10 0 . 0 0 . 0 10 0 10 0 10 1 10 1 10 2 10 2 Orbital period [days] Orbital period [days] 6 Santerne et al. (submitted)

  13. Unveiling the candidates’ nature 3 . 5 3 . 5 3 . 5 Planets Planets Planets BD Unknown Unknown Unknown 16 16 16 3 . 0 3 . 0 3 . 0 15 15 15 Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] 2 . 5 2 . 5 2 . 5 Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] 14 14 14 2 . 0 2 . 0 2 . 0 13 13 13 1 . 5 1 . 5 1 . 5 12 12 12 1 . 0 1 . 0 1 . 0 11 11 11 0 . 5 0 . 5 0 . 5 10 10 10 0 . 0 0 . 0 0 . 0 10 0 10 0 10 0 10 1 10 1 10 1 10 2 10 2 10 2 Orbital period [days] Orbital period [days] Orbital period [days] 6 Santerne et al. (submitted)

  14. Unveiling the candidates’ nature 3 . 5 3 . 5 3 . 5 3 . 5 Planets Planets Planets Planets BD BD EB Unknown Unknown Unknown Unknown 16 16 16 16 3 . 0 3 . 0 3 . 0 3 . 0 15 15 15 15 Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] 2 . 5 2 . 5 2 . 5 2 . 5 Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] 14 14 14 14 2 . 0 2 . 0 2 . 0 2 . 0 13 13 13 13 1 . 5 1 . 5 1 . 5 1 . 5 12 12 12 12 1 . 0 1 . 0 1 . 0 1 . 0 11 11 11 11 0 . 5 0 . 5 0 . 5 0 . 5 10 10 10 10 0 . 0 0 . 0 0 . 0 0 . 0 10 0 10 0 10 0 10 0 10 1 10 1 10 1 10 1 10 2 10 2 10 2 10 2 Orbital period [days] Orbital period [days] Orbital period [days] Orbital period [days] 6 Santerne et al. (submitted)

  15. Unveiling the candidates’ nature 3 . 5 3 . 5 3 . 5 3 . 5 3 . 5 Planets Planets Planets Planets Planets BD BD EB BD EB CEB Unknown Unknown Unknown Unknown Unknown 16 16 16 16 16 3 . 0 3 . 0 3 . 0 3 . 0 3 . 0 15 15 15 15 15 Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] 2 . 5 2 . 5 2 . 5 2 . 5 2 . 5 Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] 14 14 14 14 14 2 . 0 2 . 0 2 . 0 2 . 0 2 . 0 13 13 13 13 13 1 . 5 1 . 5 1 . 5 1 . 5 1 . 5 12 12 12 12 12 1 . 0 1 . 0 1 . 0 1 . 0 1 . 0 11 11 11 11 11 0 . 5 0 . 5 0 . 5 0 . 5 0 . 5 10 10 10 10 10 0 . 0 0 . 0 0 . 0 0 . 0 0 . 0 10 0 10 0 10 0 10 0 10 0 10 1 10 1 10 1 10 1 10 1 10 2 10 2 10 2 10 2 10 2 Orbital period [days] Orbital period [days] Orbital period [days] Orbital period [days] Orbital period [days] 6 Santerne et al. (submitted)

  16. Unveiling the candidates’ nature 3 . 5 3 . 5 3 . 5 3 . 5 3 . 5 3 . 5 Planets Planets Planets Planets Planets Planets BD BD EB BD EB CEB Likely planets Unknown Unknown Unknown Unknown Unknown 16 16 16 16 16 16 3 . 0 3 . 0 3 . 0 3 . 0 3 . 0 3 . 0 15 15 15 15 15 15 Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] Kepler magnitude [K p ] 2 . 5 2 . 5 2 . 5 2 . 5 2 . 5 2 . 5 Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] Transit depth [ % ] 14 14 14 14 14 14 2 . 0 2 . 0 2 . 0 2 . 0 2 . 0 2 . 0 13 13 13 13 13 13 1 . 5 1 . 5 1 . 5 1 . 5 1 . 5 1 . 5 12 12 12 12 12 12 1 . 0 1 . 0 1 . 0 1 . 0 1 . 0 1 . 0 11 11 11 11 11 11 0 . 5 0 . 5 0 . 5 0 . 5 0 . 5 0 . 5 10 10 10 10 10 10 0 . 0 0 . 0 0 . 0 0 . 0 0 . 0 0 . 0 10 0 10 0 10 0 10 0 10 0 10 0 10 1 10 1 10 1 10 1 10 1 10 1 10 2 10 2 10 2 10 2 10 2 10 2 Orbital period [days] Orbital period [days] Orbital period [days] Orbital period [days] Orbital period [days] Orbital period [days] 6 Santerne et al. (submitted)

  17. The Kepler false-positive rate of giant planets Raw ? Planets CEB BD EB 51.2% < FPR < 65.1% 7 Santerne et al. (submitted)

  18. The Kepler false-positive rate of giant planets Raw Raw Redistributed ? ? CEB Planets Planets CEB CEB Planets EB BD BD EB EB BD 51.2% < FPR < 65.1% FPR = 54.6 ± 6.5 % Fressin et al. (2013): 17.7% for all giant planets (Q1 - Q6) 7 Santerne et al. (submitted)

  19. FPP: towards smaller candidates Lower SNR ➙ FP diagnoses are less sensitive Shallower transit ➙ smaller and/or fainter contaminant or companion 8 Santerne et al. (submitted)

  20. FPP: towards smaller candidates Lower SNR ➙ FP diagnoses are less sensitive Shallower transit ➙ smaller and/or fainter contaminant or companion ➙ Absolute numbers of diluted FPs should increase ! 8 Santerne et al. (submitted)

  21. FPP: towards smaller candidates Lower SNR ➙ FP diagnoses are less sensitive Shallower transit ➙ smaller and/or fainter contaminant or companion ➙ Absolute numbers of diluted FPs should increase ! Brown (2003) 8 Santerne et al. (submitted)

  22. FPP: towards smaller candidates Lower SNR ➙ FP diagnoses are less sensitive Shallower transit ➙ smaller and/or fainter contaminant or companion ➙ Absolute numbers of diluted FPs should increase ! Multiple transits 
 ➙ very low FPP 
 (Lissauer et al., 2012,14) Brown (2003) 8 Santerne et al. (submitted)

  23. FPP: towards smaller candidates Lower SNR ➙ FP diagnoses are less sensitive Shallower transit ➙ smaller and/or fainter contaminant or companion ➙ Absolute numbers of diluted FPs should increase ! Multiple transits 
 ➙ very low FPP 
 (Lissauer et al., 2012,14) Brown (2003) Single transit 
 ➙ High FPP ? 8 Santerne et al. (submitted)

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