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Fig. 4


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).

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