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Studying exoplanets affords us the opportunity to understand the sheer diversity of planets in different physical regimes. We aim to use the statistical power of two large surveys to test and place constraints on the theoretical predictions of exoplanet atmospheric properties. We use the Spitzer Space Telescope to observe the atmospheres of a diverse sample of 34 planets in transmission and 78 planets in emission. These planets have been observed at 3.6 and 4.5 um in a systematic fashion. We study these samples in order to test the theoretical predictions of atmospheric structure and chemistry. We observe a transition in the emission spectra of ultra-hot Jupiter atmospheres at an equilibrium temperature of ~1700K. These planets exhibit even hotter daysides at 4.5 micron compared to 3.6 micron, which we attribute to seeing CO in emission due to the formation of temperature inversions, or due to a lack of redistribution from day-to-night hemispheres. Looking at the transmission spectra of the coolest close-in giant exoplanet atmospheres we find a statistical discrepancy between the observations and the predictions from 1D equilibrium chemistry models, whereby we do not see the methane expected in the coolest planets. We propose that non-equilibrium processes can lower the transition temperature between methane and CO dominated atmospheres. Finally, we compare the two observational data sets in a comprehensive manner and discuss the different physical and chemical properties probed at the different pressures.

New trends revealed by statical surveys of exoplanet atmospheres with Spitzer

Thanks Claire, a great talk! Just as a test, do you receive an email that I comment on your talk?

Hi Ignas, thanks! Sorry for the late response. Needless to say, I did not receive an email. :) 