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$\begin{figure} { \includegraphics[angle=-90,width=13.3cm,clip=]{4058.f1.eps} }\end{figure}$ Figure 1: Synthetic (dashed line) vs. observed spectrum (solid line) for BF Ori. The agreement between the photospheric and the observed median spectrum is remarkable over a large wavelength range. The extra absorption in the stronger lines (identified in the figure) is due to the circumstellar contribution. This example illustrates the need to use very faint lines to estimate the stellar parameters. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=8.8cm,clip=]{4058.f2a.eps}\includegraphics[angle=-90,width=8.8cm,clip=]{4058.f2b.eps} }\end{figure}$ Figure 2: Synthetic vs. observed spectra for SV Cep. Left: comparison of the intermediate resolution H $\alpha$ spectrum and two synthetic H $\alpha$ profiles. The best result is obtained for $T_{\rm eff}$ = 10 000 K and log g = 4.0 (blue dashed line). It was assumed that $v\sin i$ = 206 km s^-1 (Mora et al. 2001). Right: median UES spectra (solid lines) of several blends compared with the best synthetic spectra, with $T_{\rm eff}$ = 10 000 K, $v\sin i$ = 225 km s^-1 (blue dashed lines). (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=13.3cm,clip=]{4058.f3.eps} }\end{figure}$ Figure 3: The observed median UES spectrum of WW Vul (black continuous line) compared to the broadened synthetic one (blue dashed lines) in two different spectral regions. At the top of the figure, the unbroadened Kurucz model is shown with some line identifications (red solid line). (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=18cm,clip=]{4058.f4.eps} }\end{figure}$ Figure 4: Synthetic (dashed lines) vs. observed median (continuous lines) spectra of XY Per for 16 spectral features with very low CS contribution. The stellar parameters of the synthetic spectrum are given in Table 2. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=13.5cm,clip=]{4058.f5.eps} }\end{figure}$ Figure 5: Events in BF Ori. Each point corresponds to the radial velocity of one TAC and represents the average velocity $\langle v \rangle$ of the absorptions with similar radial velocities detected in different lines. $\langle v \rangle$ is a weighted average in which the higher intensity non-blended lines are assigned a weight of 1 and the rest 1/2. Error bars show the rms error of the average velocity; the numbers above the data points indicate the weighted number of lines used to estimate the average. Fractional numbers arise from the 1/2 weight attributed to some lines (see text). Redshifted events (infalling gas) are printed in red colour, while blueshifted events (outflowing gas) are in blue. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=16.2cm,clip=]{4058.f6.eps} }\end{figure}$ Figure 6: BF Ori R profiles. The normalized residual absorption profiles ( $R = 1 - F_{\rm obs}$ / $F_{\rm syn}$ ) of H $\beta$ ( left), Na I D2 and D1 ( middle) and Fe II 5018 Å ( right) are shown in the figure (black colour). The corresponding spectra are indicated in the vertical right axis (Julian and civilian epochs). The identified TACs (Gaussian components, pink colour) and the reconstructed R profile fit (blue colour) are displayed. Event numbers are shown under the Gaussians. The zero velocity interstellar components are marked as "IS''. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=13.5cm,clip=]{4058.f7.eps} }\end{figure}$ Figure 7: Events in SV Cep. Details as for Fig. 5. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=16.2cm,clip=]{4058.f8.eps} }\end{figure}$ Figure 8: SV Cep R profiles. Details as for Fig. 6. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=13.5cm,clip=]{4058.f9.eps} }\end{figure}$ Figure 9: Events in WW Vul. Events marked with a "#'' (1, 3, 4, 6, 8 and 9; red for redshifted events and blue for blueshifted events) are detected both in hydrogen and metallic lines. Events denoted with an "@'' (2, 5 and 7; green) are only seen in metallic lines. The square point of #8 in JD 1112.37 correspond to TACs only observed in Fe II and Ti II. Further details as for Fig. 5. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=16.2cm,clip=]{4058.f10.eps} }\end{figure}$ Figure 10: WW Vul R profiles. Details as for Fig. 6. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=13.5cm,clip=]{4058.f11.eps} }\end{figure}$ Figure 11: Events in XY Per. Details as for Fig. 5. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=16.2cm,clip=]{4058.f12.eps} }\end{figure}$ Figure 12: XY Per R profiles. Details as for Fig. 6. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=13cm,clip=]{4058.f13.eps} }\end{figure}$ Figure 13: Original spectrum (i.e. prior to the synthetic stellar spectrum subtraction) as observed in the JD 1023.52 spectrum of WW Vul. Wavelengths have been converted into radial velocities. Plotted lines are H $\gamma$ , H $\delta$ and the three lines of the Fe II 42 triplet. The photospheric synthetic spectrum used to form R is shown in dotted lines for H $\gamma$ and Fe II 4924 Å (being very similar for the other lines). The synthetic spectra reveal the presence of emission in the wings of H $\gamma$ and a little in the blue wing of Fe II 4924 Å. The average radial velocity $\langle v \rangle$ of the events identified after the photospheric spectrum removal and R multiGaussian fit is indicated using the same colour and label conventions of Fig. 9. There is 1 blueshifted TAC (#6, blue colour) observed both in metallic and hydrogen lines, note that $\Delta v_{H {\sc i}} \gg \Delta v_{Fe {\sc ii}}$ . There are also 2 metallic TACs (@5, @7, green) observed only in metallic lines. Event @7 can be clearly identified by visual inspection as a relatively narrow peak in the Fe II lines. In events #6 and @7 $\langle v \rangle$ does not exactly correspond with the local minima in the Fe II spectrum because the whole R profile is used in the multiGaussian fits. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} { \includegraphics[angle=-90,width=13.3cm,clip=]{4058.f3.eps} }\end{figure}$	Figure 3: The observed median UES spectrum of WW Vul (black continuous line) compared to the broadened synthetic one (blue dashed lines) in two different spectral regions. At the top of the figure, the unbroadened Kurucz model is shown with some line identifications (red solid line). (This figure is available in color in electronic form.)
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$\begin{figure} { \includegraphics[angle=-90,width=18cm,clip=]{4058.f4.eps} }\end{figure}$	Figure 4: Synthetic (dashed lines) vs. observed median (continuous lines) spectra of XY Per for 16 spectral features with very low CS contribution. The stellar parameters of the synthetic spectrum are given in Table 2. (This figure is available in color in electronic form.)
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$\begin{figure} { \includegraphics[angle=-90,width=13.5cm,clip=]{4058.f7.eps} }\end{figure}$	Figure 7: Events in SV Cep. Details as for Fig. 5. (This figure is available in color in electronic form.)
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$\begin{figure} { \includegraphics[angle=-90,width=16.2cm,clip=]{4058.f8.eps} }\end{figure}$	Figure 8: SV Cep R profiles. Details as for Fig. 6. (This figure is available in color in electronic form.)
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$\begin{figure} { \includegraphics[angle=-90,width=16.2cm,clip=]{4058.f10.eps} }\end{figure}$	Figure 10: WW Vul R profiles. Details as for Fig. 6. (This figure is available in color in electronic form.)
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$\begin{figure} { \includegraphics[angle=-90,width=13.5cm,clip=]{4058.f11.eps} }\end{figure}$	Figure 11: Events in XY Per. Details as for Fig. 5. (This figure is available in color in electronic form.)
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$\begin{figure} { \includegraphics[angle=-90,width=16.2cm,clip=]{4058.f12.eps} }\end{figure}$	Figure 12: XY Per R profiles. Details as for Fig. 6. (This figure is available in color in electronic form.)
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