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Fig. 2

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Normalized flux, squared visibility amplitudes, UD diameters, and closure phases (from top to bottom) of VY CMa obtained with the MR-K 2.1 μm mode (PA −89deg). The top panels also show fits of a UD (red) and a PHOENIX atmosphere model (blue). In these model visibility fits, the stellar component contributes ~50% of the total flux, and the remaining part is attributed to an over-resolved dust shell. The observed and model flux spectra show different slopes because of the additional dust shell that is not present in the model, and we have subtracted a best-fit linear function for a better comparison of the spectral features. The slopes that have been compensated are indicated by the dashed lines.

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