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Fig. 3


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Best fit model SEDs and photometric data points. On each figure the data and results for B275 (in black) are plotted along with one other object (in blue) for comparison. Kurucz models representing the stellar spectrum are given in dashed lines; the combined stellar and disk model in solid lines. The scattered points mark the photometry. Also indicated are the wavelength ranges of the second and first overtone bandheads. Note how B331 is both more luminous and also lacks NIR excess, with the dust emission starting around 4–5 µm.

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