Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{hiraga_0015fig1.eps} % \end{figure}$ Figure 1: The mosaic image of SNR RX J1713.7-3946 using EPIC MOS1 and MOS2 CCDs. The 17 $^\prime$ $\;\times\;$ 17 $^\prime$ square showing the Chandra FOV is also marked.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0015fig2.eps} \par\end{figure}$ Figure 2: Radial profile of the photon counts (0.7-2.0 keV) for the white-dashed rectangle region shown in Fig. 1. It is integrated over the vertical dimension.
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In the text

$\begin{figure} \par\includegraphics[width=13.2cm,clip]{0015fig3.eps} \end{figure}$ Figure 3: a) The numbered regions have been selected for the spectral analysis of the rim region and the dashed squares have been selected for the spectral analysis of the interior region. The dashed black curves denote the background region for NW and SW observations, respectively. b) A and B are two sets of 10 rectangle regions selected for examination of the possible spectral variation in the radial direction. The named regions of NWb, NWd, SWb and SWd have been selected for estimating absolute fluxes (Sect. 3.3). The apparent circular shape of the inner rim is also depicted.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{0015fig4} \end{figure}$ Figure 4: Representative spectra obtained by all CCD detectors, MOS1 (black), MOS2 (red) and pn (green) are shown as characteristic examples for the rim region a) and the interior region b). In both a) and b), MOS1 spectra are scaled by a factor 0.5 for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=14.2cm,clip]{0015fig5} \par\end{figure}$ Figure 5: Results of spectral fits with an absorbed power-law model for selected regions in the western bright portion depicted by filled circles. From top to bottom, we have plotted the best-fit values (with their 90% errors) of photon index, $\Gamma$ , absorbing column density, $N_{\rm H}$ in units of $10^{22}~{\rm cm}^{-2}$ , unabsorbed flux in 1.0-10 keV band in units of $10^{-12} ~{\rm erg~cm^{-2}~s^{-1}~arcmin^{-2}}$ , and $\chi ^2_{\nu }$ . The resultant $\Gamma$ and $\chi ^2_{\nu }$ when adopting a fixed $N_{\rm H}$ of 0.78 $\times~10^{22}~{\rm cm^{-2}}$ are shown by open circles in the top and bottom panels, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{0015fig6} \par\end{figure}$ Figure 6: Best-fit parameter distribution of $\Gamma$ ( left) and $N_{\rm H}$ ( right) both for the rim region (solid line) and the interior region (dashed line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{0015fig7} \par\end{figure}$ Figure 7: Spectrum of the interior region (same data as shown in Fig. 4b) with the best-fit model containing a thermal component in addition to the absorbed power-law model.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{0015fig8}\end{figure}$ Figure 8: Radial profiles for two sets of 10 rectangle regions, A) and B) (depicted in Fig. 3b). The dashed curves correspond to three possible shell thickness profilesassuming a uniform distribution of the volume emissivity (see text for further description).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0015fig9}\end{figure}$ Figure 9: The same figure as Fig. 2 of Fukui et al. (2003). The CO distribution in a velocity range of -11 to $-3~ {\rm km~s^{-1}}$ is depicted by the pink contours. The TeV $\gamma$ -ray significance map is superposed as the yellow contours. The X-ray image is also shown; it is the soft band image obtained by XMM-Newton as shown in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{hiraga_0015fig1.eps} % \end{figure}$	Figure 1: The mosaic image of SNR RX J1713.7-3946 using EPIC MOS1 and MOS2 CCDs. The 17 $^\prime$ $\;\times\;$ 17 $^\prime$ square showing the Chandra FOV is also marked.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0015fig2.eps} \par\end{figure}$	Figure 2: Radial profile of the photon counts (0.7-2.0 keV) for the white-dashed rectangle region shown in Fig. 1. It is integrated over the vertical dimension.
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$\begin{figure} \par\includegraphics[width=16.4cm,clip]{0015fig4} \end{figure}$	Figure 4: Representative spectra obtained by all CCD detectors, MOS1 (black), MOS2 (red) and pn (green) are shown as characteristic examples for the rim region a) and the interior region b). In both a) and b), MOS1 spectra are scaled by a factor 0.5 for clarity.
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$\begin{figure} \par\includegraphics[width=13.6cm,clip]{0015fig6} \par\end{figure}$	Figure 6: Best-fit parameter distribution of $\Gamma$ ( left) and $N_{\rm H}$ ( right) both for the rim region (solid line) and the interior region (dashed line).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{0015fig7} \par\end{figure}$	Figure 7: Spectrum of the interior region (same data as shown in Fig. 4b) with the best-fit model containing a thermal component in addition to the absorbed power-law model.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{0015fig8}\end{figure}$	Figure 8: Radial profiles for two sets of 10 rectangle regions, A) and B) (depicted in Fig. 3b). The dashed curves correspond to three possible shell thickness profilesassuming a uniform distribution of the volume emissivity (see text for further description).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0015fig9}\end{figure}$	Figure 9: The same figure as Fig. 2 of Fukui et al. (2003). The CO distribution in a velocity range of -11 to $-3~ {\rm km~s^{-1}}$ is depicted by the pink contours. The TeV $\gamma$ -ray significance map is superposed as the yellow contours. The X-ray image is also shown; it is the soft band image obtained by XMM-Newton as shown in Fig. 1.
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