$\begin{figure} \par\includegraphics[width=18.5cm,clip]{8644fig1.eps}\end{figure}$ Figure 1: V2051 Oph average out-of-eclipse spectrum. All lines are double-peaked with prominent emission from the Balmer and He I lines. He II and Fe II lines are also in emission, albeit weaker.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{8644fig3.eps}\end{figure}$ Figure 3: V2051 Oph trailed spectrograms. The x-axis represents the velocity in km s^-1 and the y-axis the orbital phase. The grayscale contrast has been adjusted to emphasise between emission (black) and absorption (white).
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8644fig4.eps} \end{figure}$ Figure 4: Modulation of the double-peaks separation. Superimposed is the dominant periodicity of $P_{\rm orb}/2$ .
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8644fig5.eps}\end{figure}$ Figure 5: Radial extension of all emission lines. Dashed lines correspond to the refined outer radii when the tidal effect is taken into account.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{8644fig6.eps}\end{figure}$ Figure 6: V2051 Oph Doppler maps. Top to bottom rows correspond to the Balmer lines, He I lines and the Fe II triplet, respectively. The x and y axis represent the V_x and V_y velocities respectively, spanning from -1500 to 1500 $\rm km ~\rm s^{-1}$ . Each row has its own intensity scale.
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In the text

$\begin{figure} \par\includegraphics[width=18.5cm,clip]{8644fig1.eps}\end{figure}$	Figure 1: V2051 Oph average out-of-eclipse spectrum. All lines are double-peaked with prominent emission from the Balmer and He I lines. He II and Fe II lines are also in emission, albeit weaker.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{8644fig2.eps} \end{figure}$	Figure 2: V2051 Oph trailed spectra of the 11 most prominent lines. The spectra have been ordered according to phase.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{8644fig3.eps}\end{figure}$	Figure 3: V2051 Oph trailed spectrograms. The x-axis represents the velocity in km s^-1 and the y-axis the orbital phase. The grayscale contrast has been adjusted to emphasise between emission (black) and absorption (white).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{8644fig4.eps} \end{figure}$	Figure 4: Modulation of the double-peaks separation. Superimposed is the dominant periodicity of $P_{\rm orb}/2$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{8644fig5.eps}\end{figure}$	Figure 5: Radial extension of all emission lines. Dashed lines correspond to the refined outer radii when the tidal effect is taken into account.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{8644fig6.eps}\end{figure}$	Figure 6: V2051 Oph Doppler maps. Top to bottom rows correspond to the Balmer lines, He I lines and the Fe II triplet, respectively. The x and y axis represent the V_x and V_y velocities respectively, spanning from -1500 to 1500 $\rm km ~\rm s^{-1}$ . Each row has its own intensity scale.
Open with DEXTER