tokens: and white to strongest continuum flux). The actual phases of observation are indicated by arrows on the right hand side. The similar line of C iv λ 1550.774 appears offset to higher velocity. Both features are formed mainly in the wind of the Be star, but shell variations are present on the high velocity side of the core. Figure 3.12. Al ii λ1670. The top panel shows the individual spectra of Al ii λ 1670.7867 plotted as a function of radial velocity and orbital phase (such that the continuum is aligned with the phase of observation). The spectral flux depth relative to the continuum is indicated by the scale bar in upper right. The lower panel shows the same interpolated in orbital phase and portrayed as a gray scale image (black corresponding to deepest absorption and white to strongest continuum flux). The actual phases of observation are indicated by arrows on the right hand side. Figure 3.13. Al iii λ1854. The top panel shows the individual spectra of Al iii λ 1854.7164 plotted as a function of radial velocity and orbital phase (such that the continuum is aligned with the phase of observation). The spectral flux depth relative to the continuum is indicated by the scale bar in upper right. The lower panel shows the same interpolated in orbital phase and portrayed as a gray scale image (black corresponding to deepest absorption and white to strongest continuum flux). The actual phases of observation are indicated by arrows on the right hand side. Figure 3.14. Al iii λ1862. The top panel shows the individual spectra of Al iii λ 1862.7895 plotted as a function of radial velocity and orbital phase (such that the continuum is aligned with the phase of observation). Thespectral flux depth relative to the continuum is indicated by the scale bar in upper right. The lower panel shows the same interpolated in orbital phase and portrayed as a gray scale image (black corresponding to deepest absorption and white to strongest continuum flux). The actual phases of observation are indicated by arrows on the right hand side. Figure 3.15. Fe iii λ1895. The top panel shows the individual spectra of Fe iii λ 1895.46 plotted as a function of radial velocity and orbital phase (such that the continuum is aligned with the phase of observation). The spectral flux depth relative to the continuum is indicated by the scale bar in upper right. The lower panel shows the same interpolated in orbital phase and portrayed as a gray scale image (black corresponding to deepest absorption and white to strongest continuum flux). The actual phases of observation are indicated by arrows on the right hand side. The lines of Fe iii λ λ 1895.46, 1896.814 also appear in the figure. Figure 3.16. Mg ii λ2796. The top panel shows the individual spectra of Mg ii λ 2796.352 plotted as a function of radial velocity and orbital phase (such that the continuum is aligned with the phase of observation). The spectral flux depth relative to the continuum is indicated by the scale bar in
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