All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1371fig1.ps} \end{figure}$ Figure 1: The spectrum of V630 Sgr is dominated by Balmer and He II lines in emission.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{1371fig2.ps} \end{figure}$ Figure 2: With the double logarithmic scaling it becomes obvious that two slopes are needed to fit the continuum of V630 Sgr. While the red part of the continuum yields a value of $\alpha = -2.5$ , the blue part is fitted with $\alpha = -1.2$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{1371fig3.ps} \end{figure}$ Figure 3: Apart from the Balmer series in emission, the spectrum of XX Tau shows various low ionisation lines like He I and Fe II. He II is only present at 469 nm.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1371fig4.ps} \end{figure}$ Figure 4: The spectrum of V529 Ori is dominated by an extremely red continuum and the strong H $\alpha$ line in emission.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{1371fig5.ps} \end{figure}$ Figure 5: Although the spectrum of CQ Vel is rather noisy, the blue continuum together with the presence of Balmer and He II lines in emission confirm the identification of this object as an old nova.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{1371fig6.ps} \end{figure}$ Figure 6: Spectrum of V842 Cen. The upper plot shows the spectrum as observed are notable. The blue continuum and the various strong emission lines (hydrogen, He I, He II). The strongest Balmer lines have been plotted individually to compare the line profiles; the contamination of H $\alpha$ with N II becomes obvious. To check for the fainter lines, the continuum has been subtracted in the lower plot. Several weak, high excitation lines become visible, which probably originate in the hot nova shell, which is still present seventeen years after the explosion.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1371fig1.ps} \end{figure}$	Figure 1: The spectrum of V630 Sgr is dominated by Balmer and He II lines in emission.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{1371fig2.ps} \end{figure}$	Figure 2: With the double logarithmic scaling it becomes obvious that two slopes are needed to fit the continuum of V630 Sgr. While the red part of the continuum yields a value of $\alpha = -2.5$ , the blue part is fitted with $\alpha = -1.2$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{1371fig3.ps} \end{figure}$	Figure 3: Apart from the Balmer series in emission, the spectrum of XX Tau shows various low ionisation lines like He I and Fe II. He II is only present at 469 nm.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1371fig4.ps} \end{figure}$	Figure 4: The spectrum of V529 Ori is dominated by an extremely red continuum and the strong H $\alpha$ line in emission.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{1371fig5.ps} \end{figure}$	Figure 5: Although the spectrum of CQ Vel is rather noisy, the blue continuum together with the presence of Balmer and He II lines in emission confirm the identification of this object as an old nova.
Open with DEXTER