Photometry and Spectroscopy of Exoplanetary Atmospheres

1. Photometry and Spectroscopy of Exoplanetary Atmospheres Joseph Harrington University of Central Florida Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech) Happy Birthdays, Sara (7/20) and Jay (7/19, age 6)!

2. UCF Planetary Sciences • University of Central Florida – ORLANDO! • 6th-largest US undergraduate univ., 50,100, growing • PhD in Physics, Planetary Sciences Track • Planetary Sciences Professors: (Search soon!) • Humberto Campins (comets) • Daniel Britt (surfaces) • Yanga Fernandez (comets) • Joseph Harrington (exoplanets & atmospheres) • Joshua Colwell (rings, ice, dust) • Robert Peale (high-T molecular spectroscopy) • Eduardo Martin (brown dwarfs & exoplanets) • Self-funded, soft-money: (Interested? Talk to jh!) • Csaba Palotai (atmospheres)

3. Lessons of Planetary Science • Every planet is different – unlike stars! • Big compositional differences, no dominant process • Chaos reigns in orbits, meteorology, geophysics • There will never be an H-R diagram for planets! • In new situations, “good” models often fail • Assumptions no longer hold • E.g., Over half the weather models can't do Venus's 4-day winds Exoplanetary Science Models vastly underconstrained All measured exoplanets far outside SS phase space

4. Modelers permitted (funded) to: • Explore exotic conditions for first time • Pulsar planets • Radical forcing (Hot Jupiters and Neptunes) • Fe, enstatite clouds and rain • Triaxial atmospheric geometry • Atmospheric chemical latent heat cycles • Diamond/ocean planets, interior cooling problems • Orbital dynamics, habitability, formation... • Eliminate large areas of modeling phase space

5. Secondary Eclipses

6. Secondary Eclipses

7. First Direct Detection I Deming, Seager, Richardson, Harrington (2005, Nature) HD 209458 b, Spitzer MIPS, 24 µm 1.5 h pre-eclipse, 3 h eclipse, 1.5 h post-eclipse F24 m = 55 ± 10 Jy (10-26 W/m2/Hz) FP/F* = 0.0026 ± 0.00046 TB,24 m = 1130 ± 150 K tSE = t=0 + P/2 ± 7 min Significant orbital eccentricity very unlikely Inflated radius not likely due to tidal heating

8. Data Deming et al. (2005b)

9. First Direct Detection II! Charbonneau et al. (2005, ApJ) submitted TrES-1 the same day! Spitzer IRAC, 4.5 and 8 µm simultaneously FP/F*: 4.5 µm: 0.00066 ± 0.00013, 8 µm: 0.00225 ± 0.00036 Tb = 1060 ± 50 K A = 0.31 ± 0.14 e = 0 Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech)

10. S/N Champ: HD 189733 b K1-K2 star (small, cool), close (19.3 pc), V = 7.67 Rp = 1.26 RJup (bigish for a hot Jupiter) Many times higher S/N than HD 209458 b Deming et al. (2006, ApJ 644, 560)

11. Measuring Atmospheres A planet's spectrum tells its story. Take Mars:

12. Broadband Photometry Knutson et al. (2008, ApJ) HD 209458b Spitzer 3.6, 4.5, 5.7, 8 In eclipse Day-side emission Inversion H2O evidence

13. Broadband Photometry HD 189733b (Charbonneau et al.), no inversion XO-1b (Machalek et al.) A few planets are nice, but... ... we need enough to do statistics This means looking at lower S/N

14. Spitzer ToO Program Collaborate with all willing discovery teams Observe all planets w/ good Spitzer S/N 60 hr/year Cycles 3-5, 200 hr Warm Spitzer Cycle 6 Fill in plot of Tb vs.Teq WASP 1,2,3,8,12,...; HAT 1,2,7; GJ 436b; CoRot 2, others Legacy: Lightcurves derived from optimal pipeline

15. 8-m Eclipses

16. GJ 436b

17. GJ 436b

18. Pixel-Phase Effect

19. Direct Measurements after Harrington et al. (2007)

20. Phase Curves Ups And b w/ Spitzer MIPS Non-transiting planet 5 epochs around orbit Big variation! Radiation beats advection after Harrington et al. (2006, Science)

21. Phase Curves HD 189733b IRAC 8-μm Small variation Temperature more homogenized 24-μm MIPS Also GJ 436b, HD 149026b Knutson et al. (2007, Nature)

22. Phase Curves HD 80606b IRAC 8-μm High e! 828F* vari Pseudosynch. rotation Secondary! 4+-hr rad. time constant Laughlin et al. (2009, Nature)

23. Spectroscopy: Thermal +? Spitzer IRS, eclipse HD 209458b: Richardson et al. (2007, Nature) Continuum seen Intriguing peaks HD 189733b: Grillmair et al. (2007, ApJ) Continuum seen No peaks

24. Blame the Dark Stuff Some planets have an absorbing material (TiO/VO)? Absorbs ~all incoming light Makes inversion/stratosphere Emits strongly in near-mid IR, forms photosphere rad << advect: Instantaneous reradiation Implies a colder back side – strong dynamical forcing Other planets have more uniform T T isn't the only factor in forming absorber Variability on HD 149026b? Mira-like process for forming/destroying TiO? What energy input varies?

25. Combined-Light Mission EPOXI, SOFIA, warm Spitzer, CoRoT, Kepler, JWST, MOST, ground-based,: none optimized for exoplanet characterization Room for a dedicated probe-scale mission 1-2 m, closed-cycle cooling, hides behind solar panel Near-mid-IR point-source spectrophotometer Good on-board calibration sources, 100-day stability Much better/more appropriate measurements possible

26. UCF Winter School 2010! Exoplanets for Planetary Scientists 6-8 January 2010 (Wed – Fri) UCF Campus, Orlando, Florida, USAhttp://planets.ucf.edu/winterschool2010 Advanced-grad-level “school” talks Apply planetary theory to exoplanet cases Nuts-and-bolts exoplanet observing Oral and poster sessions with latest exoplanet results Showcase results to planetary science community Great place to pick up planetary collaborators!

27. Jupiter Impact Last Night Impact discovered 2009-07-19 before 13:30 UTC Discovered by amateur Anthony Wesley, Australia No impact 8 hours earlier Morphology very like SL9 http://jupiter.samba.org/ jupiter-impact.html 15-year anniversary of SL9

28. Jupiter Impact Last Night Glenn Orton (JPL) was observing Jupiter at IRTF Confirms high-altitude material in methane images

29. Jupiter Impact Last Night Weak methane-band image (889 nm) from Portugal Confirms high-altitude material