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Fig. 33


Expected radial plot for Large Program sources, if the expectation is based on the two brightest targets, Circinus galaxy and NGC 1068. For this figure, these two targets have been “placed” at respective distances and times as far away as they actually are so that their flux matches the median flux of the weak sources. At these distances, baselines much longer than those offered at the VLTI (black/gray: maximum baseline using UTs/ATs) would be needed to resolve the elongated disk component that has been found with MIDI in these two bright and nearby sources.

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