Notes. Equations for the intensity profiles, I(μ), and the corresponding complex visibilities, V, are given. In these equations, μ(= cos(θ)) is the cosine of the angle θ between thedirection perpendicular to the stellar surface and the direction toward a distant observer. For a line-of-sight starting at the center and moving toward the limb of the stellar disk, μ varies between 1 and 0. Also, Γ is the gamma function and is the Bessel function of first kind and of order ν_λ. The dimensionless variable z is given by π⊘B_p∕λ, where B_p (= |B_p|) is the interferometric baseline length projected onto the target, λ is the effective wavelength of the observation, and ⊘ is the stellarangular diameter for the considered LD model. In an interferometric study of a given star, as is the case here, one generally seeks to observe at several spatial frequencies for a good uv coverage, with observations performed on many different realizations of the vector B_p∕λ = (u, v), as in Fig. 1.