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Fig. A.1


Spectral energy distribution (black line) of our best fit model, compared to dereddened photometry (AV = 0.3, Q11) from the literature (Q11, Tilling et al. 2012; Cutri et al. 2011; Ishihara et al. 2010; Egan et al. 2003; Helou & Walker 1988). The stellar photosphere is shown as the thin dashed line.

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