$\begin{figure} \includegraphics[width=8.8cm,clip]{3127f1.eps} \end{figure}$ Figure 1: Optical light curve of WeCAPP-N2000-03 in R (grey circles) and I (black triangles). The I band data show a negative bias as the reference image contained nova epochs.
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In the text

$\begin{figure} \includegraphics[width=8.8cm,clip]{3127f2.ps} \end{figure}$ Figure 2: Part of the Chandra HRC I image of observation 1912 used for the source catalogue of K2002. Circles with 5'' radius indicate nova positions. The cross indicates the M 31 center, the aim point of the observation.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=17cm,clip]{3127f3.ps} \par\end{figure}$ Figure 3: Light curves for M 31 and M 33 novae that were detected within 1000 d after outburst. Detections of individual novae are connected by solid lines, and connections to upper limits are marked by dashed lines. The light curve from nova V1974 Cyg is adapted from Krautter et al. (1996) assuming 1 cts s $^{-1} = 0.2 \times 10^{36}$ erg s^-1.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{3127f4.ps} \end{figure}$ Figure 4: XMM-Newton EPIC spectrum of source [PFH2005] 191 (Nova in M 31 [SI2001] 1992-01) for observation s1. The absorbed black body fit to the data (see Sect. 3.1) is shown in the upper panel.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{3127f5.ps} \end{figure}$ Figure 5: XMM-Newton EPIC spectrum of source [PFH2005] 320 (nova in M 31 WeCAPP-N2000-03) for observation c3. The absorbed black body fit to the data (see Sect. 3.9) is shown in the upper panel.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{3127f6.ps} \end{figure}$ Figure 6: XMM-Newton EPIC spectrum of source [PFH2005] 395 (nova in M 31 Jul-98) for observation c4. The absorbed bremsstrahlung fit to the data (see Sect. 3.15) is shown in the upper panel. The reduced flux in the pn spectrum is due to the location of the source on a CCD gap.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{3127f7.ps} \end{figure}$ Figure 7: Histogram of the number of optical novae per year in M 31 contained in the nova catalogue used for X-ray cross-correlation (see Sect. 2). The number of optical novae showing X-ray emission is indicated coded for ROSAT and XMM-Newton/ Chandra. The time span of X-ray observations is indicated.
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In the text

$\begin{figure} \includegraphics[width=8.8cm,clip]{3127f1.eps} \end{figure}$	Figure 1: Optical light curve of WeCAPP-N2000-03 in R (grey circles) and I (black triangles). The I band data show a negative bias as the reference image contained nova epochs.
Open with DEXTER

$\begin{figure} \includegraphics[width=8.8cm,clip]{3127f2.ps} \end{figure}$	Figure 2: Part of the Chandra HRC I image of observation 1912 used for the source catalogue of K2002. Circles with 5'' radius indicate nova positions. The cross indicates the M 31 center, the aim point of the observation.
Open with DEXTER

$\begin{figure} \includegraphics[angle=-90,width=17cm,clip]{3127f3.ps} \par\end{figure}$	Figure 3: Light curves for M 31 and M 33 novae that were detected within 1000 d after outburst. Detections of individual novae are connected by solid lines, and connections to upper limits are marked by dashed lines. The light curve from nova V1974 Cyg is adapted from Krautter et al. (1996) assuming 1 cts s $^{-1} = 0.2 \times 10^{36}$ erg s^-1.
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$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{3127f4.ps} \end{figure}$	Figure 4: XMM-Newton EPIC spectrum of source [PFH2005] 191 (Nova in M 31 [SI2001] 1992-01) for observation s1. The absorbed black body fit to the data (see Sect. 3.1) is shown in the upper panel.
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$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{3127f5.ps} \end{figure}$	Figure 5: XMM-Newton EPIC spectrum of source [PFH2005] 320 (nova in M 31 WeCAPP-N2000-03) for observation c3. The absorbed black body fit to the data (see Sect. 3.9) is shown in the upper panel.
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$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{3127f6.ps} \end{figure}$	Figure 6: XMM-Newton EPIC spectrum of source [PFH2005] 395 (nova in M 31 Jul-98) for observation c4. The absorbed bremsstrahlung fit to the data (see Sect. 3.15) is shown in the upper panel. The reduced flux in the pn spectrum is due to the location of the source on a CCD gap.
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$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{3127f7.ps} \end{figure}$	Figure 7: Histogram of the number of optical novae per year in M 31 contained in the nova catalogue used for X-ray cross-correlation (see Sect. 2). The number of optical novae showing X-ray emission is indicated coded for ROSAT and XMM-Newton/ Chandra. The time span of X-ray observations is indicated.
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