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$\begin{figure} \par\epsfig{file=Fd073_f1.eps,width=8.8cm,height=4.5cm,clip} \end{figure}$ Figure 1: EPIC-PN spectrum of IGR J16320-4751 and residuals to the absorbed powerlaw model.
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In the text

$\begin{figure} \par\epsfig{file=Fd073_f2.eps,width=8.8cm,height=4cm,clip}\end{figure}$ Figure 2: Left: error contours for the column density ( $N_{\rm H}$ ), and the photon index ( $\Gamma$ ) obtained from the XMM-Newton observation. The cross marks the location of the best fit values, and the 68% ( $\Delta \chi ^2=2.30$ ) and 90% ( $\Delta \chi ^2=4.61$ ) contours are shown. Right: same plot for the ASCA observation.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{Fd073_f3.ps}\par \end{figure}$ Figure 3: Upper panel: 0.5-12 keV PN light curve of IGR J16320-4751 measured after background subtraction. The time sampling is 50 s, which shows the fast rise during the flare episodes. The lower panels represent a zoom on the region of the flares (starting around relative time 1500 s). The 2-5 keV, 5-12 keV and hardness ratio between 2-5 and 5-12 keV are shown. The time sampling is 200 s.
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In the text

$\begin{figure} \par\epsfig{file=Fd073_f4.ps,width=6cm,height=5cm,clip} \end{figure}$ Figure 4: 2-MASS K-band $2.5\times 2$ $^{\prime }$ image of IGR J16320-4751 field, the XMM error circle is superimposed. One can clearly see the two possible counterparts. 1 stands for the most probable one, and 2 for the second.
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In the text

$\begin{figure} \par\epsfig{file=Fd073_f1.eps,width=8.8cm,height=4.5cm,clip} \end{figure}$	Figure 1: EPIC-PN spectrum of IGR J16320-4751 and residuals to the absorbed powerlaw model.
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$\begin{figure} \par\epsfig{file=Fd073_f2.eps,width=8.8cm,height=4cm,clip}\end{figure}$	Figure 2: Left: error contours for the column density ( $N_{\rm H}$ ), and the photon index ( $\Gamma$ ) obtained from the XMM-Newton observation. The cross marks the location of the best fit values, and the 68% ( $\Delta \chi ^2=2.30$ ) and 90% ( $\Delta \chi ^2=4.61$ ) contours are shown. Right: same plot for the ASCA observation.
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$\begin{figure} \par\includegraphics[width=8.8cm]{Fd073_f3.ps}\par \end{figure}$	Figure 3: Upper panel: 0.5-12 keV PN light curve of IGR J16320-4751 measured after background subtraction. The time sampling is 50 s, which shows the fast rise during the flare episodes. The lower panels represent a zoom on the region of the flares (starting around relative time 1500 s). The 2-5 keV, 5-12 keV and hardness ratio between 2-5 and 5-12 keV are shown. The time sampling is 200 s.
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$\begin{figure} \par\epsfig{file=Fd073_f4.ps,width=6cm,height=5cm,clip} \end{figure}$	Figure 4: 2-MASS K-band $2.5\times 2$ $^{\prime }$ image of IGR J16320-4751 field, the XMM error circle is superimposed. One can clearly see the two possible counterparts. 1 stands for the most probable one, and 2 for the second.
Open with DEXTER