Upper panel: best-fitting specific intensity model for three different assumed planetary radii. The specific intensity used for creating an artificial observation is shown as a dashed line. The stellar model is taken from case 2 in Table 1 at λ = 1.60 μm. Note that the x-axis is the projected linear distance from the center of the star, rather than the more commonly used μ-angle. Middle panel: synthetic light curves from derived specific intensity and assumed planetary radius. The artificial observation is shown as black dots, and the theoretical noiseless transit curve is shown as a dashed line. Lower panel: differences squared between observed flux and best possible fit increase as the assumed planetary radius moves away from Rp = 1. The best possible fit is achieved close to the correct value.