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

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

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

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

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

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

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

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

10. HD 149026

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

12. Hot Jupiter atmospheres?

13. 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:

14. 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

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

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

17. What about chemistry? Need IR observations: GL 229B (BD) T dwarf IR opacities dominated by CH 4, H 2 O. Oppenheimer, B. et al. 1998, ApJ, 502, 932

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

19. Ground? Challenge is the Earth’s atmosphere! Limits only just beginning to reach sufficient sensitivity. CO Search Terrestrial CH 4 Deming, D. et al. 2005, ApJ, 622, 1149