Best-fit resolved fluxes given as a function of wavelength, assuming that β Pic emits as a blackbody of temperature 8200 K. The solid lines give the flux expected from blackbody sources of various equilibrium temperatures and the optimum emitting surface area (computed by χ² minimisation). The dashed line represents the flux from a blackbody source of 8200 K or, equivalently, from scattered stellar light (). The K-band flux obtained from archival VLTI/VINCI measurements is shown for comparison but is not included in the fit (see more information in the main text).