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Ge/Ay133

What can transit observations tell us about (exo)-planetary science?. Ge/Ay133. Sometimes the absence of signal is interesting:. Gilliland, R.L. et al. 2000, ApJ, 545, L47. No transits in 47 Tuc, `expectation’=30-40 (34,000 stars). Transits, approach #1:. Sato, B. et al. 2005, ApJ,

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Ge/Ay133

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  1. What can transit observations tell us about (exo)-planetary science? Ge/Ay133

  2. Sometimes the absence of signal is interesting: Gilliland, R.L. et al. 2000, ApJ, 545, L47 No transits in 47 Tuc, `expectation’=30-40 (34,000 stars)

  3. Transits, approach #1: Sato, B. et al. 2005, ApJ, astro-ph/0507009 Search for transits in systems known to have planets at the doppler crossings.

  4. Photometry is fairly straightforward: Amateur observations of HD 209458 b Bruce L. Gary, Santa Barbara, CA Arto Oksanen SBIG cameras, Meade telescopes, V filters

  5. Transits, approach #2: TrES-1 Search for transits in many stars using a suite of low cost robotic telescopes. Alonso, R. et al. 2004, ApJ, 613, L153

  6. Photometry from space can be extremely good: Brown, T.M. et al. 2001, ApJ, 552, 699 HD 209458 - HST The KEPLER mission is dedicated to photometry and can search for earth mass planets in the so- called habitable zone. www.kepler.arc.nasa.gov

  7. Transits and the Rossiter-McLaughlin effect (1924): Winn, J.N. et al. 2005, ApJ, 631, 1215

  8. A comparison of transiting planet systems: Remember, size is not a strong function of mass, so very accurate measurements are needed!

  9. HD 149026

  10. Secondary ecplises in the IR with Spitzer, see photons from the hot Jupiters! T = 1060 ± 50 K A = 0.31 ± 0.14 Charbonneau, D. et al. 2005, ApJ, 626, 523

  11. Hot Jupiter atmospheres?

  12. M L T In the optical/near-IR, the spectra of M → T dwarfs (similar temp. as the hot Jupiters) show strong alkali metal lines:

  13. First detection of an extrasolar planet atmosphere: Look for the transit depth in filters on and off the Na D-line with HST. Charbonneau, D. et al. 2001, ApJ, 568, 377

  14. Vidal-Madjar, A. et al. 2004, ApJ, 604, L69 Atmospheres Part II: Most atoms have their so called resonance lines in the UV. The H I depth is VERY large. EXOSPHERE?

  15. Rowe, J.F.. et al. 2006, ApJ, 646, 1241 Secondary eclipses can also put limits on the visible albedo. The MOST satellite finds A(HD209458b)<0.25 (1s) (Jupiter=0.5, 300-700 nm). Why so dark?

  16. What about chemistry? Need IR observations: GL 229B (BD) Oppenheimer, B. et al. 1998, ApJ, 502, 932 T dwarf IR opacities dominated by CH4, H2O.

  17. Spitzer phtometry and IR atmospheric models: Charbonneau, D. et al. 2005, ApJ, 626, 523

  18. Ground? Challenge is the Earth’s atmosphere! Terrestrial CH4 CO Search Limits only just beginning to reach sufficient sensitivity. Deming, D. et al. 2005, ApJ, 622, 1149

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