All Figures

$\begin{figure} \par\includegraphics[angle=90,width=7.9cm,clip]{5390f1.ps}\end{figure}$ Figure 1: Upper panel: broad band fluxed spectrum of Mrk 279. The data have been binned by a factor of two. Lower panel: signal to noise ratio for the unbinned spectrum.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.75cm,clip]{5390f2.ps}\end{figure}$ Figure 2: LETGS light curve of Mrk 279 in the zeroth spectral order. Bin size: 1000 s. The individual 7 time segments are labeled at the bottom. The FUSE and HST pointings are also marked.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{5390f3.ps}\end{figure}$ Figure 3: Percentage deviation from the parameter values of the combined spectrum (Table 2) for: the power-law slope, $\Gamma$ , the power-law 2-10 keV luminosity, the temperature ( kT) and the luminosity of the modified black body. The horizontal axis labels the observation number as defined in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.65cm,clip]{5390f4.ps}\end{figure}$ Figure 4: Residuals, in terms of sigma, to the continuum model in the O VII triplet region. A broad Gaussian (dashed line) has been added only to guide the eye. The continuum is represented by a power-law plus a modified black body absorbed by galactic absorption. The labels refer to the position of expected absorption/emission narrow lines.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.4cm,clip]{5390f5.ps}\end{figure}$ Figure 5: The spectral energy distribution for Mrk 279. The points at 1000 and 1350 Å are the continuum flux of the simultaneous FUSE and HST-STIS observation, respectively. The X-ray continuum is taken from the present LETGS data.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{5390f6.ps}\end{figure}$ Figure 6: Best fit of the intrinsic luminosity of the UV broad emission lines ( upper panel). The model is displayed by a continuous line only to guide the eye. Lower panel: residuals in terms of $\sigma$ to the best fit.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{5390f7.ps}\end{figure}$ Figure 7: Best fit luminosity profiles of eight of the ions considered for the fit. The luminosity was integrated at each radius using the weighting function $n^{\beta }$ . For each emission line the diamonds indicate the luminosity-weighted radius. Note that the model underpredicts theobserved luminosity of C IV by $\sim$ 40%.
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In the text

$\begin{figure} \par\includegraphics[height=13.65cm,width=4.7cm,angle=90,clip]{53... ... \includegraphics[height=13.7cm,width=5cm,angle=90,clip]{5390f8d.ps}\end{figure}$ Figure 8: Lower panel: best fit to the LETGS spectrum of Mrk 279 divided per wavelength range. The broad emission, predicted by the LOC fitting, and the narrow emission features, shifted up of a factor 2 for plotting purpose, are also overplotted. Upper panel: absorbing components: Dark dashed and light dot-dashed line: z=0 absorbers. Warm absorber: light solid line ( $\log\xi=0.47$ ), dark solid line ( $\log\xi=2.49$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.5cm,clip]{5390f9.ps}\end{figure}$ Figure 9: Detail of the O VIII absorption line, fitted with only one component ( $\log\xi=0.47$ , dashed line) and with two components ( $\log\xi=0.47,2.49$ , solid line).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.45cm,clip]{5390f10.ps}\end{figure}$ Figure 10: The hydrogen column density as a function of the ionization parameter determined for: single ions (individual points) and an $N_{\rm H}$ continuous distribution model (solid line). See Sect. 2.4.2 for a full description.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.35cm,clip]{5390f11.ps}\end{figure}$ Figure 11: Comparison between the 4th and the 5th segment of Mrk 279 observation (Fig. 2). The 4th spectrum (continuum line with asterisks) is normalized to the unabsorbed continuum of the 5th observation. The 5th spectrum is plotted with the light-solid line.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.55cm,clip]{5390f12.ps}\end{figure}$ Figure 12: The pressure ionization parameter vs. the electron temperature. The two components of the warm absorber for Mrk 279 are indicated as squares.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.9cm,clip]{5390f1.ps}\end{figure}$	Figure 1: Upper panel: broad band fluxed spectrum of Mrk 279. The data have been binned by a factor of two. Lower panel: signal to noise ratio for the unbinned spectrum.
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$\begin{figure} \par\includegraphics[angle=90,width=7.75cm,clip]{5390f2.ps}\end{figure}$	Figure 2: LETGS light curve of Mrk 279 in the zeroth spectral order. Bin size: 1000 s. The individual 7 time segments are labeled at the bottom. The FUSE and HST pointings are also marked.
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$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{5390f3.ps}\end{figure}$	Figure 3: Percentage deviation from the parameter values of the combined spectrum (Table 2) for: the power-law slope, $\Gamma$ , the power-law 2-10 keV luminosity, the temperature ( kT) and the luminosity of the modified black body. The horizontal axis labels the observation number as defined in Fig. 2.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=7.65cm,clip]{5390f4.ps}\end{figure}$	Figure 4: Residuals, in terms of sigma, to the continuum model in the O VII triplet region. A broad Gaussian (dashed line) has been added only to guide the eye. The continuum is represented by a power-law plus a modified black body absorbed by galactic absorption. The labels refer to the position of expected absorption/emission narrow lines.
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$\begin{figure} \par\includegraphics[angle=90,width=7.4cm,clip]{5390f5.ps}\end{figure}$	Figure 5: The spectral energy distribution for Mrk 279. The points at 1000 and 1350 Å are the continuum flux of the simultaneous FUSE and HST-STIS observation, respectively. The X-ray continuum is taken from the present LETGS data.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{5390f6.ps}\end{figure}$	Figure 6: Best fit of the intrinsic luminosity of the UV broad emission lines ( upper panel). The model is displayed by a continuous line only to guide the eye. Lower panel: residuals in terms of $\sigma$ to the best fit.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{5390f7.ps}\end{figure}$	Figure 7: Best fit luminosity profiles of eight of the ions considered for the fit. The luminosity was integrated at each radius using the weighting function $n^{\beta }$ . For each emission line the diamonds indicate the luminosity-weighted radius. Note that the model underpredicts theobserved luminosity of C IV by $\sim$ 40%.
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$\begin{figure} \par\includegraphics[angle=90,width=7.5cm,clip]{5390f9.ps}\end{figure}$	Figure 9: Detail of the O VIII absorption line, fitted with only one component ( $\log\xi=0.47$ , dashed line) and with two components ( $\log\xi=0.47,2.49$ , solid line).
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$\begin{figure} \par\includegraphics[angle=90,width=7.45cm,clip]{5390f10.ps}\end{figure}$	Figure 10: The hydrogen column density as a function of the ionization parameter determined for: single ions (individual points) and an $N_{\rm H}$ continuous distribution model (solid line). See Sect. 2.4.2 for a full description.
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$\begin{figure} \par\includegraphics[angle=90,width=7.35cm,clip]{5390f11.ps}\end{figure}$	Figure 11: Comparison between the 4th and the 5th segment of Mrk 279 observation (Fig. 2). The 4th spectrum (continuum line with asterisks) is normalized to the unabsorbed continuum of the 5th observation. The 5th spectrum is plotted with the light-solid line.
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$\begin{figure} \par\includegraphics[angle=90,width=7.55cm,clip]{5390f12.ps}\end{figure}$	Figure 12: The pressure ionization parameter vs. the electron temperature. The two components of the warm absorber for Mrk 279 are indicated as squares.
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