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We explored two aspects of the problem of characterizing cool extrasolargiant planets in scattered optical light with a space based coronagraph. First,for a number of the known radial velocity (RV) giants we computed traditionalforward models of their atmospheric structure and clouds, given various inputassumptions, and computed model albedo spectra. Such models have been computedbefore, but mostly for generic planets. Our new models demonstrate that thereis likely interesting spectral diversity among those planets that are mostfavorable for direct detection. Second, we applied a powerful Markov ChainMonte Carlo (MCMC) retrieval technique to synthetic noisy data of cool giantsto better understand how well various atmospheric parameters--particularlymolecular abundances and cloud properties--could be constrained. This is thefirst time such techniques have been applied to this problem. The process istime consuming, so only a dozen or so cases could be completed in the limitedtime available. Nevertheless the results clearly show that even at S/N ~ 5,scientifically interesting and valuable conclusions can be drawn about theproperties of giant planet atmospheres from noisy spectra. We find thatatmospheric abundances are best constrained when the planet gravity is bounded.Thus direct imaging observations of known radial velocity planets are extremelyvaluable as limits on a target planet's gravity can be obtained fromastrometric imaging and reflectivity and mass-radius relationship arguments(for mass and radius, respectively). Further retrieval studies are clearlywarranted and would be valuable to help guide instrument design decisions.

A Quick Study of the Characterization of Radial Velocity Giant Planets in Reflected Light by Forward and Inverse Modeling