[@brown01], but to distinguish a difference at the 4-$\sigma$ level in the planetary transit radius in and out of the Na-D line at 0.589 . In this way, neutral sodium atoms were discovered in HD209458b’s atmosphere [@Charbonneau02; @SeagerSasselov00; @Hubbard01]. Though indirect, this is the first measurement of the composition of the atmosphere of an extrasolar planet. Since then, the Lyman-$\alpha$ line of hydrogen has similarly been detected in HD209458b’s atmosphere [@vidal], and by the large magnitude ($\sim$15%) of the photometric dip at this UV wavelength ($\lambda$) a planetary wind[@lunine95] comprised of molecular break-up products has been inferred. However interesting, transits are rare and no substitute for direct imaging and optical and infrared spectra. Spectra can provide diagnostics for atmospheric composition, radius, gravity, and mass. Images are ground truth for the existence of a planet and provide orbital information that complements that gleaned from Doppler measurements. Furthermore, direct detection might be able to distinguish the different models of giant planet formation, such as nucleation around an ice/rock core[@mizuno] and direct collapse[@boss], and can probe the outer orbits where the majority of EGPs might reside.

Since the indirect radial-velocity technique for EGP discovery selects for the closer variety, it is likely that 