All Figures

$\begin{figure} \par\includegraphics[angle=0,width=14cm,clip]{2367fig1.ps}\end{figure}$ Figure 1: Left panel: XMM-MOS1 image of the Vela PWN in the 3-10 keV band; contour levels are at $5~\times~10^{-4}$ , $1~\times~10^{-3}$ , $2~\times~ 10^{-3}$ and $8~\times~10^{-3}$ times the brightest point. Right panel: MECS image of the source; outer contour levels are at $3\times 10^{-3}$ , $7\times 10^{-3}$ , $13\times 20^{-3}$ and $33\times 10^{-3}$ times the brightest point. Note the more extended emission in the south-west and south-east regions.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2367fig2.ps}\end{figure}$ Figure 2: Panel a): the power law photon index in the 3-10 keV band of MOS (stars) and MECS (filled circles) spectra at varying extraction radius. Panel b): the power law photon indices in the 3-10 keV band of MOS spectra extracted from the annuli listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2367fig3.ps}\end{figure}$ Figure 3: Vela PWN flux in the 3-10 keV band at varying extraction radius.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2367fig4.ps}\end{figure}$ Figure 4: Best fit values of f_MP in the combined log-parabolic fit with the PDS at varying extraction radius.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2367fig5.ps}\end{figure}$ Figure 5: Best fit of MECS and PDS data with a broken power law model ( $15^{\prime }$ extraction radius for the MECS data). See Table 2 for the best fit parameter values.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2367fig6.ps}\end{figure}$ Figure 6: The optical to X-ray spectral energy distribution of the Vela PWN compared with other literature results. Our SEDs are the broken power law (solid and short-dashed lines) and the log-parabola (dotted line) to which are superposed the deconvolved spectral data. The thick solid line is the spectrum measured by the Birmingham 2 experiment (Willmore et al. 1992) and the dotted lines represent the broken power law SED rescaled to the flux measured by the MECS with an extraction radius of 4'. The thick long dashed line is the broad band spectrum of the compact nebula based on OSSE data (De Jager 1996) and used by by Sefako & De Jager (2003). Optical upper limits (empty triangles) are taken from Mignani et al. (2003) extrapolated to an area of 10⁴ arcsec² to cover all the inner part of the plerion. The triangles in the $\gamma$ -ray band represent EGRET upper limits from Kanbach et al. (1994).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2367fig2.ps}\end{figure}$	Figure 2: Panel a): the power law photon index in the 3-10 keV band of MOS (stars) and MECS (filled circles) spectra at varying extraction radius. Panel b): the power law photon indices in the 3-10 keV band of MOS spectra extracted from the annuli listed in Table 1.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2367fig3.ps}\end{figure}$	Figure 3: Vela PWN flux in the 3-10 keV band at varying extraction radius.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2367fig4.ps}\end{figure}$	Figure 4: Best fit values of f_MP in the combined log-parabolic fit with the PDS at varying extraction radius.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2367fig5.ps}\end{figure}$	Figure 5: Best fit of MECS and PDS data with a broken power law model ( $15^{\prime }$ extraction radius for the MECS data). See Table 2 for the best fit parameter values.
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