Dynamically consistent analysis of Galactic WN4b stars

This database contains appendix B of the paper "Dynamically consistent analysis of Galactic WN4b stars" by Lefever et al., accepted for publication in Astronomy & Astrophysics, with article reference aa58211-25.Appendix B: Spectral fitsWe perform quantitative spectroscopy using PoWRhd modelling on the six following stars: WR1, WR6, WR7, WR18, WR37 andWR58. The “by-eye” fits per star are shown in the figures B1-6, where the blue spectra represent the observation, while the red spectra represent the best-fit models. The SEDs are displayed along with relevant photometry on the top of each figure, while the UV and optical normalised fluxes are shown in the remaining panels. Where there is observed IR data available (WR6 and WR 37), the He I 1.084 μm line is shown as well. The normalised spectra are supplemented with relevant line labels, where the SED panel in each figure contains observational information on the distances and on the reddening applied to each target. Below is a short description for each figure: Fig. B1: The SED (top panel), UV (second panel) and optical (bottom two panels) spectra of WR1. Fig. B2: The SED (top panel), UV (second panel) and optical (bottom two panels) spectra of WR6. The bottom right panel shows the IR He I 1.084 μm line. Fig. B3: The SED (top panel), UV (second panel) and optical (bottom two panels) spectra of WR7. Fig. B4: The SED (top panel), UV (second panel) and optical (bottom two panels) spectra of WR18. Fig. B5: The SED (top panel), UV (second panel) and optical (bottom two panels) spectra of WR37. The bottom right panel shows the IR He I 1.084 μm line. Fig. B6: The SED (top panel), UV (second panel) and optical (bottom two panels) spectra of WR58.