Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4257F1.PS} \end{figure}$ Figure 1: Image of NGC 4593 taken with the UVW1 filter of the Optical Monitor onboard of XMM- Newton. Besides the bright core the spiral arm structure is visible.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F2.PS} \end{figure}$ Figure 2: Fit residuals of a power-law fit to the LETGS data for NGC 4593, clearly showing a dip in the spectrum between 10 and 18 Å and the strong soft excess above 18 Å. The power-law was fit between 2 and 10 Å and the data are binned by a factor of 10.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F3.PS} \end{figure}$ Figure 3: Power-law plus modified black body fit (thin solid line) and the model including the xabs components as described in Table 2 (thick solid line) to the LETGS data. The thin line at about 0.002 counts s^-1 Å^-1 is the subtracted background contribution. For clarity the data are binned by a factor of 5. Instrumental edges are labeled, as well as the O VII forbidden line.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F4.PS} \end{figure}$ Figure 4: Detailing the 10-17 Å region of Fig. 3. Power-law and modified black body fit (thin solid line) and the fit including the xabs components (thick solid line) to the unbinned LETGS data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F5.PS} \end{figure}$ Figure 5: Detail of the RGS data (upper panel) and the LETGS data (lower panel). In the LETGS panel the absorption lines are indicated, G stands for Galactic absorption. In the upper panel the instrumental features for the RGS are labeled. The subtracted background is indicated for the LETGS data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F6.PS} \end{figure}$ Figure 6: Fit to the RGS data with model 6 of Table 4. For clarity RGS 1 and RGS 2 were binned by a factor of 10 and added. The relativistic N VII Ly $\alpha$ line is indicated by N VII Ly $\alpha$ written horizontally. The features labeled Inst. are periodic dips due to CCD-gaps, or due to instrumental calibration.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F7.PS} \end{figure}$ Figure 7: Fit residuals between 23.5 and 26.5 Å, showing the observed excess at the N VII Ly $\alpha$ wavelength, which is fitted in model 6 (Table 4) with a relativistic emission line.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F8.PS} \end{figure}$ Figure 8: The relative fit residuals with respect to a simple power-law fit for the pn and MOS2 data added together. The power-law was fit between 2 and 10 keV.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{H4257F9.PS} \end{figure}$ Figure 9: The light curve for the LETGS data, in the zeroth spectral order. Note the rise phase between 70 and 97 ks, and the peak phase between 97 and 105 ks.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F10.PS} \end{figure}$ Figure 10: The light curve during the rise and peak phase for the LETGS data, but now split up into three wavelength bands. The stars joined by the thick line represent the power-law component, or the 1-10 Å photons. The crosses represent the soft excess component, i.e. the 20-40 Å photons and the open circles joined by a thin line are the intermediate wavelength range of 10-20 Å. The errors for the power-law and intermediate component are similar to those plotted for the soft excess component.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4257F1.PS} \end{figure}$	Figure 1: Image of NGC 4593 taken with the UVW1 filter of the Optical Monitor onboard of XMM- Newton. Besides the bright core the spiral arm structure is visible.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F2.PS} \end{figure}$	Figure 2: Fit residuals of a power-law fit to the LETGS data for NGC 4593, clearly showing a dip in the spectrum between 10 and 18 Å and the strong soft excess above 18 Å. The power-law was fit between 2 and 10 Å and the data are binned by a factor of 10.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F3.PS} \end{figure}$	Figure 3: Power-law plus modified black body fit (thin solid line) and the model including the xabs components as described in Table 2 (thick solid line) to the LETGS data. The thin line at about 0.002 counts s^-1 Å^-1 is the subtracted background contribution. For clarity the data are binned by a factor of 5. Instrumental edges are labeled, as well as the O VII forbidden line.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F4.PS} \end{figure}$	Figure 4: Detailing the 10-17 Å region of Fig. 3. Power-law and modified black body fit (thin solid line) and the fit including the xabs components (thick solid line) to the unbinned LETGS data.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F5.PS} \end{figure}$	Figure 5: Detail of the RGS data (upper panel) and the LETGS data (lower panel). In the LETGS panel the absorption lines are indicated, G stands for Galactic absorption. In the upper panel the instrumental features for the RGS are labeled. The subtracted background is indicated for the LETGS data.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F6.PS} \end{figure}$	Figure 6: Fit to the RGS data with model 6 of Table 4. For clarity RGS 1 and RGS 2 were binned by a factor of 10 and added. The relativistic N VII Ly $\alpha$ line is indicated by N VII Ly $\alpha$ written horizontally. The features labeled Inst. are periodic dips due to CCD-gaps, or due to instrumental calibration.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F7.PS} \end{figure}$	Figure 7: Fit residuals between 23.5 and 26.5 Å, showing the observed excess at the N VII Ly $\alpha$ wavelength, which is fitted in model 6 (Table 4) with a relativistic emission line.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4257F8.PS} \end{figure}$	Figure 8: The relative fit residuals with respect to a simple power-law fit for the pn and MOS2 data added together. The power-law was fit between 2 and 10 keV.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{H4257F9.PS} \end{figure}$	Figure 9: The light curve for the LETGS data, in the zeroth spectral order. Note the rise phase between 70 and 97 ks, and the peak phase between 97 and 105 ks.
Open with DEXTER