Comparison of Hubble data (black) with single B-type star model (orange) and binary Be+Bstr model (magenta), as summarized in Table 4, with the main contributing species labeling specific absorption features. Top panel: illustrates the good fit of both models to the G430M data, with the binary model being a better fit to the hydrogen line cores and to the He I 4026 Å line, as indicated by the residuals plotted below the spectra. Also shown are the models of Simón-Díaz et al. (2020, grey) and Shenar et al. (2020, blue). Lower panel: compares the FUV data (same color coding) illustrating that, for example, the Fe III complex of lines around 1900 Å is much too strong in the Shenar et al. (2020) model. Neither interstellar lines nor disk emission are included in the models.