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Directed Follow-Up of Gaia Photometry in Search of Transiting Planets

Directed Follow-Up of Gaia Photometry in Search of Transiting Planets. Shay Zucker Yifat Dzigan Tel-Aviv University. Dzigan & Zucker , MNRAS, 415, 2513, 2011 Dzigan & Zucker , ApJL , 753, L1, 2012 Dzigan & Zucker ,, MNRAS, accepted.

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Directed Follow-Up of Gaia Photometry in Search of Transiting Planets

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  1. Directed Follow-Up of Gaia Photometry in Search of Transiting Planets Shay Zucker YifatDzigan Tel-Aviv University • Dzigan & Zucker, MNRAS, 415, 2513, 2011 • Dzigan & Zucker, ApJL, 753, L1, 2012 • Dzigan & Zucker,, MNRAS, accepted

  2. Aposteriori Detection of HD209458b in Hipparcos Data Söderhjelm 1999 Robichon & Arenou 2000 Castellano et al. 2000

  3. Why not a real detection? • No one believed it was possible • Photometry not precise enough • Low cadence Can we use the data for detection somehow?

  4. Directed Follow-Up – General Idea • Actually sampled transits provide some knowledge about the period, phase, duration and depth of a hypothetical transit, if it exists. • Using MCMC we can present this scarce information as a Probability Distribution Function over (P,Tc,w,d) (assuming a BLS-like model). • For each future time – t, we can use this PDF to calculate an instantaneous transit probability – ITP(t) • Each new follow-up observataion is added and the process is repeated.

  5. Could HD209458b have been detected in 2004?

  6. Could HD209458b be detected in 2004?

  7. Could HD209458b be detected in 2004?

  8. Lessons from Hipparcos HD209458Exercise • With five sampled transits, low cadence data, augmented by DFU, allow detection. • Data become useless after a few years. • For completeness – we should mention HD189733b.

  9. Testing DFU on Gaia • Simulated Gaia light curves inspired by known transiting planets (period and duration, coordinates) • Gaia scanning law • Phase chosen to produce required number of sampling transits • Photon noise level – 1 mmag. • We defined three scenarios of detection.

  10. First Scenario – Gaia data alone • Gaia samples enough transits to allow detection of the transit using only Gaia data. • 1-mmag precision makes this scenario possible. • Simulation inspired by CoRoT-1b (P=1.51 d, w=0.1 d) • Assuming five sampled transits (Ntot=64) • d > 0.005 mag

  11. First Scenario – Gaia data alone

  12. Second Scenario – one DFU observation • Gaia samples enough transits to allow several possible solutions. One DFU observation is enough to constrain the period. • Simulation inspired by CoRoT-4b (P=9.20 d, w=0.16 d) • Assuming three sampled transits (Ntot=63) • d > 0.001 mag

  13. Second Scenario – one DFU observation

  14. Third Scenario – Few DFU Observations • Gaia samples enough transits to allow several possible solutions. A few DFU observations are needed to constrain the period. • Simulation inspired by WASP-4b (P=1.338 d, w=0.104 d) • Assuming four sampled transits (Ntot=83) • d= 0.005 mag

  15. Third Scenario – Few DFU Observations

  16. Third Scenario – Few DFU Observations Only Gaia data Gaia data + 1 DFU observation Gaia data + 2 DFU observations

  17. We shouldn’t wait till the last minute • ITP deteriorates over time • Therefore – we should start observing even before the end of the mission • Tres-1b, (P=3.03 d, w=0.104 d) • Three sampled tranists (Ntot=48) (mid-life of mission) • Assume d=0.008 mag

  18. Is it worth it? Observational Window Function 70 Gaia Measurements 130 Gaia Measurements

  19. Is it worth it? • Assuming 2 hr transit, Galactic model, transiting planet statistics from complete surveys (OGLE) • Down to 14th G magnitude: minimum 7 transits: ~70 transiting HJs and VHJs minimum 5 transits: ~200 minimum 3 transits: ~600 • Down to 16thG magnitude: minimum 7 transits: ~300 transiting HJs and VJHs minimum 5 transits: ~900 minimum 3 transits: ~2600

  20. To do list: • Get organized • Dedicated observatory network? • CU7 follow-up network? • Science Alert team? • Prescreening scheme (metallicity, brightness, activity etc.) • Develop a more efficient computational scheme than MCMC. • Objective criteria for applying DFU • Wald statistics • ITP values • ITP skewness • Smaller planets (Neptunian and below?) • Other low-cadence surveys

  21. Additional slides Contingencies for potential questions

  22. HD189733 – Hipparcos and DFU observations

  23. HD189733 – Hipparcos and DFU observations

  24. HD189733 – Hipparcos and DFU observations

  25. HD189733 – Hipparcos and DFU observations

  26. Sanity checks

  27. Gaia WASP-4b – degradation of ITP over 10 years

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