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Fig. 7


The observed Spitzer/IRS spectrum (Backman et al. 2009) (small dots) and the modeled SED of the inner region. Top: planet “A”, middle: planet “B”, bottom: without a planet. Thin lines: contributions of the different size bins to the SED, thick line: the total emission from all sizes. The size distribution slope q and the dust mass ℳdust are the same as in Fig. 5.

This figure is made of several images, please see below:

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