Surface of Titan : model and VIMS observations

In this presentation we will describe how we explain the surface reflectivity observed by DISR and how we retrieved the surface albedo of Titan from VIMS observation, showing where are the main uncertainties. We show that the reflectivity at the Huygens Landing Site may be explained a layer of liquid methane at the surface. We also show that other zones on Titan may have the same type of surface reflectivity than the HLS.