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Fig. 10


Absolute flux distributions of our program stars (gray lines) compared to the final photospheric models (blue lines). The models include absorption by interstellar hydrogen Lyman lines and reddening according to the column densities nH and E(BV) values as given in the panels. For clarity, models and observations were smoothed with Gaussians with a full width at half maximum of 0.3 Å.

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