Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig1.ps} \end{figure}$ Figure 1: The rebinned spectrum of NGC 5548 as taken with the LETGS instrument in 1999 (upper) 2002 (middle) and 2005 (lower).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig2.ps} \includegraphics[angle=-90,width=8.4cm,clip]{9862fig3.ps} \end{figure}$ Figure 2: Total oxygen column densities as measured with the LETGS instrument in 2002 (rectangles) and 2005 (diamonds). 1 $\sigma$ errors are shown as well, apart from ions for which an upper limit to the total column density can be measured (arrows). The upper panel shows the total column densities for which the velocity broadening $\sigma$ was allowed to vary, the lower panel where $\sigma$ was fixed to the values of Steenbrugge et al. (2005).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig4.ps} \end{figure}$ Figure 3: The Fe K ${\alpha }$ emission line fit for the 2005 observation.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig5.ps} \end{figure}$ Figure 4: Comparison of the 1999 (diamonds), 2002 (solid line) and 2005 (rectangles) spectra, close to the forbidden O VII emission line at 22.101 $\AA$ . The deep O V absorption line is visible at 22.354 $\AA$ . The 1999 and 2005 spectra have been scaled to the 2002 flux.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig6.ps} \end{figure}$ Figure 5: RXTE lightcurve of NGC 5548, rebinned to one month intervals, spanning from 1996 till 2007. The count rate shown is per PCU detector of the RXTE. All 6 spectral observations (see Table 2) are shown as well. There is a gap in the data from the beginning of 2003 till 2004, when the source was not monitored by RXTE. The errors in the countrates are at the 1% level.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig1.ps} \end{figure}$	Figure 1: The rebinned spectrum of NGC 5548 as taken with the LETGS instrument in 1999 (upper) 2002 (middle) and 2005 (lower).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig4.ps} \end{figure}$	Figure 3: The Fe K ${\alpha }$ emission line fit for the 2005 observation.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig5.ps} \end{figure}$	Figure 4: Comparison of the 1999 (diamonds), 2002 (solid line) and 2005 (rectangles) spectra, close to the forbidden O VII emission line at 22.101 $\AA$ . The deep O V absorption line is visible at 22.354 $\AA$ . The 1999 and 2005 spectra have been scaled to the 2002 flux.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9862fig6.ps} \end{figure}$	Figure 5: RXTE lightcurve of NGC 5548, rebinned to one month intervals, spanning from 1996 till 2007. The count rate shown is per PCU detector of the RXTE. All 6 spectral observations (see Table 2) are shown as well. There is a gap in the data from the beginning of 2003 till 2004, when the source was not monitored by RXTE. The errors in the countrates are at the 1% level.
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