Portraits of distant worlds

This thesis presents observational studies of the atmospheres of extrasolar planets, including the first longitudinal temperature profile of an extrasolar planet and the first detection of a temperature inversion in the atmosphere of an extrasolar planet. Our observations target four eclipsing gas-giant planets known as "hot Jupiters"; as a result of their short orbital periods we expect these planets to be tidally locked, with day-night circulation patterns and atmospheric chemistries that differ significantly from those of Jupiter. The first two chapters of this thesis describe infrared observations of the secondary eclipses of HD 209458b and TrES-4 with the Spitzer Space Telescope . By measuring the decrease in flux as the planet passes behind its parent star, we can characterize the infrared emission spectra of these planets and from that learn something about their dayside pressure-temperature profiles. Our observations reveal that these two planets have spectra with water bands in emission, requiring the presence of an atmospheric temperature inversion between 0.1 - 0.01 bars. The third chapter describes a ground-based search for thermal emission from TrES-1 using L -band grism spectroscopy with the NIRI instrument on Gemini North. Unlike Spitzer photometry, which is limited to broad bandpasses at these wavelengths, grism spectroscopy offers the opportunity to resolve specific features in the planetary emission spectrum. We find that our precision is limited by our ability to correct for time-varying slit losses from pointing drift and seeing changes, and place an upper limit on the depth of the planet's secondary eclipse in this band. The fourth and fifth chapters describe observations of the infrared phase variations of the hot Jupiter HD 189733b in the 8 and 24 μm Spitzer bands. By monitoring the changes in the brightness of this planet as it rotates around its parent star we can determine how much energy is circulated from the perpetually-illuminated day side around to the night side. We then invert these data to produce a longitudinal temperature profile for the planet, allowing us to resolve the locations of prominent hot and cold regions in the planet's atmosphere.