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Fig. C.3.


Binned and dereddened IUE spectra (black) of HR 6819. They are scaled to 55% to represent the flux contribution from the inner B3 III component to the total flux; spectra plotted in gray indicate 35−75% ranges (Appendix C.4.) The theoretical SED for Teff = 16 kK and log g = 3.5 (Castelli & Kurucz 2003) is overplotted in red, multiplied by 6.2 × 10−18 to account for distance and stellar radius.

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