All Figures

	Figure 1: Average wavelets power spectral density (WPSD) of the 464 processed interferograms of NGC 1068. The subtraction of the background noise from the processed fringes' power peak left no residual bias on the final WPSD. The power integration is done between wave numbers 2000 and 8000 cm-1.
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In the text

Figure 2: Synthetic squared visibility function for (dashed line) a 5 mas Gaussian, (dashed-dotted line) a 30 mas Gaussian, and (solid lines) two examples for a two-component model where (upper line/ lower line) 56%/40% of the total flux comes from a 3 mas/0.1 mas Gaussian and the remaining 44%/60% from a 54 mas/42 mas Gaussian ( FWHM values). Measurements are available for baselines B=46 m reported in this letter (marked by the -symbol with error bar) and up to B=6-10 m (Wittkowski et al. 1998; Weinberger et al. 1999; Weigelt et al. 2004). Both measurements are only matched if the small component has a size clearly below 5 mas and if only part of the total flux in our FOV arises from this 5 mas component, and another part from a larger component. It is assumed that the FOV is the same for all shown models.

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In the text