Fig. 8
Section of the VFTS 358 spectrum showing, from left-to-right, the Hϵ, N II λ3995, and He I λλ4009, 4026 lines; we note that Hϵ is complicated by absorption from the interstellar Ca H line (as well as nebular emission). Model spectra for our adopted physical parameters and 12 + log (N/H) = 6.9, 7.7, and 8.5, are overplotted in red, green, and blue, respectively.
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