All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1154_fig1.ps} \end{figure}$ Figure 1: EPIC pn spectra (double background subtraction) of the SW and SE regions of SNR RX J1713.7-3946. The fit with a power-law model gives $N_{{\rm H}}=0.71 \pm 0.02 \times 10^{22}$ cm^-2 and $\Gamma = 2.33 \pm 0.03$ for the SW region and $N_{{\rm H}}=0.57 \pm 0.03 \times 10^{22}$ cm^-2 and $\Gamma = 2.16 \pm 0.06$ for the SE region at a 90% confidence level.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1154_fig2.eps}\hspace*{3mm} \includegraphics[width=7.8cm,clip]{1154_fig3.eps} \end{figure}$ Figure 2: Left panel: MOS mosaiced image of SNR RX J1713.7-3946 in the 0.8-2 keV energy band. Right panel: same as left panel but in the 2-10 keV energy band. The neutron star 1WGA J1713.4-3949 is located in the middle of the CE pointing. Both images were adaptively smoothed to a signal-to-noise ratio of 10. The scaling is square root with the higher cut fixed to 30% of the SNR maximum X-ray brightness. The color bar numbers are in units of counts/s/pixel with a pixel size of $4\hbox {$^{\prime \prime }$ }$ . The bad resolution in the NE is due to a very short exposure time (see Table 1). Moreover, it is possible that the smoothing has removed a few small-scale features in this NE pointing.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1154_fig4.eps} \end{figure}$ Figure 3: 1.4 GHz ATCA radio image (courtesy of J.S. Lazendic) overlaid with the 2-10 keV contour of SNR RX J1713.7-3946. The scaling is linear. The contour values start at 10^-5 MOS counts/s/pixel and are square root spaced up to $1.9 \times 10^{-3}$ counts/s/pixel with a pixel size of $4\hbox {$^{\prime \prime }$ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1154_fig5.eps}\hspace*{6mm... ...ps}\hspace*{6mm} \includegraphics[width=7.9cm,clip]{1154_fig8.eps} \end{figure}$ Figure 4: Left panel: absorbing column map $N_{{\rm H}}$ (in units of 10²² cm^-2) overlaid with the contour of the 2-10 keV image of SNR RX J1713.7-3946. The contour values start at 10^-5 MOS counts/s/pixel and are square root spaced up to $1.9 \times 10^{-3}$ counts/s/pixel with a pixel size of $4\hbox {$^{\prime \prime }$ }$ . The big boxes of our adaptive grid found in the NE and NW pointings are due to the low exposure time there. Right panel: photon index map overlaid with the same X-ray contours. In both images, the scaling is linear.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1154_fig9.ps}\vs... ...*{3mm} \includegraphics[angle=-90,width=7.5cm,clip]{1154_fig10.ps} \end{figure}$ Figure 5: Top panel: pn spectra of two SW regions of similar brightness ( $\sim$ $2.8 \times 10^{-4}$ photons/cm²/s/keV/arcmin²) and same photon index ( $\Gamma \sim 2.4$ ) but with different absorbing column densities. The absorbing column is $1.09\pm {0.05} \times 10^{22}$ cm^-2 for the top spectrum (17h11m58.2s, -39 $^{\circ }$ 59 $\hbox {$^\prime $ }$ 44.5 $\hbox {$^{\prime \prime }$ }$ ) and $0.77\pm {0.05} \times 10^{22}$ cm^-2 for the other one (17h11m52.5s, -39 $^{\circ }$ 55 $\hbox {$^\prime $ }$ 54.6. $\hbox {$^{\prime \prime }$ }$ ). Bottom panel: pn spectra of two SW regions of similar brightness ( $\sim$ $2 \times 10^{-4}$ photons/cm²/s/keV/arcmin²) and same absorbing column ( $N_{{\rm H}} \sim 0.9 \times 10^{22}$ cm^-2) but with different photon index. $\Gamma = 2.07\pm {0.10}$ for the top spectrum (17h12m26.7s, -39 $^{\circ }$ 57 $\hbox {$^\prime $ }$ 34.4 $\hbox {$^{\prime \prime }$ }$ ) and $\Gamma = 2.66\pm {0.12}$ for the other one (17h11m52.6s, $-39^{\circ }$ 54 $\hbox {$^\prime $ }$ 49.0 $\hbox {$^{\prime \prime }$ }$ ).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1154_fig11.ps} \end{figure}$ Figure 6: Correlation plot between the absorbing column $N_{{\rm H}}$ (in units of 10²² cm^-2) and the normalized brightness at 1 keV. Each point corresponds to the value found for a particular pixel of the mapping grid (Sect. 2.3.4) and the error bars are given at a 90% confidence level. The symbols are defined as follow (cf. Table 1): $\Box$ for NE, for NW, $\bullet$ for SW, $\circ$ for SE, $\triangle$ for CE. The regions which are the more absorbed are the brightest. They are mainly located in the SW. The regions which have small $N_{{\rm H}}$ are the less bright and are found in the CE and SE.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1154_fig12.ps}\par\vspace*{3mm} \includegraphics[width=8cm,clip]{1154_fig13.ps} \end{figure}$ Figure 7: Top panel: correlation plots at the shock location in the SW ( $\bullet$ ) and SE ( $\circ$ ) regions between the absorbing column $N_{{\rm H}}$ (in units of 10²² cm^-2) and the normalized brightness at 1 keV (in units of 10^-4 photons/cm²/s/keV/arcmin²). Each point corresponds to the value found for a particular pixel of the mapping grid (Sect. 2.3.4) and the error bars are given at a $90\%$ confidence level. The points of the SW region are selected so that they are above $2.0 \times 10^{-4}$ photons/cm²/s/keV/arcmin². Bottom panel: correlation plots between the photon index $\Gamma$ and the normalized brightness at 1 keV for the same set of points as above. The error bars are given at a $90\%$ confidence level.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1154_fig14.eps}\hspace*{4m... ...e*{4mm} \includegraphics[width=8cm,height=1cm,clip]{1154_fig17.eps} \end{figure}$ Figure 8: Left panel: spatial distribution of the hardness ratio [0.7-0.9 keV]/[1.0-1.3 keV] overlaid with the contour of the 2-10 keV image of SNR RX J1713.7-3946. Right panel: spatial distribution of the hardness ratio [5-8 keV]/[1.6-2.0 keV] overlaid with the same X-ray contours. In both images, the point-like sources have been removed. The scaling is linear. Regions of extraction used for the search of the thermal emission are shown and labeled from 1 to 8.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1154_fig18.ps} \end{figure}$ Figure 9: For each of the 8 regions considered (see Fig. 8), changes of the parameters ( $N_{{\rm H}}$ , $\Gamma$ ) with the addition of a thermal component. The star correspond to the power-law model (cf. Table 2). The black triangle correspond to the power-law plus thermal equilibrium model (cf. Table 3). The error bars are given at a $90\%$ confidence level.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1154_fig19.ps} \end{figure}$ Figure 10: EPIC spectra of the central source 1WGA J1713.4-3949 of the SNR RX J1713.7-3946 (MOS1 in black, MOS2 in red and pn in green). Best-fit obtained with a double blackbody model.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1154_fig20.eps} \end{figure}$ Figure 11: Optical image between 2300 and 3000 Å (Second Generation Digitized Sky Survey in red color at 450-600 THz) overlaid with the contour of the 2-10 keV X-ray image of SNR RX J1713.7-3946. The scaling is linear with the higher cut fixed at $5 \sigma$ of the mean optical brightness value.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1154_fig21.ps} \end{figure}$ Figure 12: Correlation plot between the absorbing column $N_{{\rm H}}$ (in units of 10²² cm^-2) and the normalized optical brightness. To obtain this plot, the optical image shown in Fig. 11 has been cut following the absorbing column map grid. Each point corresponds to the value found for a particular pixel of the mapping grid (Sect. 2.3.4) and the error bars are given at a $90\%$ confidence level. The symbols are defined as in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{1154_fig22.ps}\psfrag{NH}{$N_{{\rm H}}$ }\end{figure}$ Figure 13: Top panel: the cumulative absorbing column density as obtained from the atomic and molecular hydrogen, as a function of radial velocity. The continuous line corresponds to the average NH estimated towards the NW region, the dotted line corresponds to the SW region and the dashed line to a line-of-sight directed to 1WGA J1713.4-3949. Bottom panel: the rotation curve towards l=347.5, b=-0.5 as obtained from Fich et al.'s (1989) circular galactic rotation model.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1154_fig23.ps} \end{figure}$ Figure 14: Average CO spectra obtained towards the NW (continuous line) and towards the SW (dotted line) from the CfA CO survey (Dame et al. 2001). The SW emission is higher than the NW emission for LSR velocities between 0 and -10 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1154_fig24.ps} \end{figure}$ Figure 15: Kinetic energy of the explosion as a function of the SNR age for several solar masses of the supernova ejecta ( $M_{{\rm ej}} = 10, 15$ and $20 ~ {M}_{\odot}$ ) and different ambient medium densities ( $n_0 = 5 \times 10^{-3}, 1 \times 10^{-3}$ and $5 \times 10^{-4}$ cm^-3).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1154_fig1.ps} \end{figure}$	Figure 1: EPIC pn spectra (double background subtraction) of the SW and SE regions of SNR RX J1713.7-3946. The fit with a power-law model gives $N_{{\rm H}}=0.71 \pm 0.02 \times 10^{22}$ cm^-2 and $\Gamma = 2.33 \pm 0.03$ for the SW region and $N_{{\rm H}}=0.57 \pm 0.03 \times 10^{22}$ cm^-2 and $\Gamma = 2.16 \pm 0.06$ for the SE region at a 90% confidence level.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1154_fig4.eps} \end{figure}$	Figure 3: 1.4 GHz ATCA radio image (courtesy of J.S. Lazendic) overlaid with the 2-10 keV contour of SNR RX J1713.7-3946. The scaling is linear. The contour values start at 10^-5 MOS counts/s/pixel and are square root spaced up to $1.9 \times 10^{-3}$ counts/s/pixel with a pixel size of $4\hbox {$^{\prime \prime }$ }$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1154_fig18.ps} \end{figure}$	Figure 9: For each of the 8 regions considered (see Fig. 8), changes of the parameters ( $N_{{\rm H}}$ , $\Gamma$ ) with the addition of a thermal component. The star correspond to the power-law model (cf. Table 2). The black triangle correspond to the power-law plus thermal equilibrium model (cf. Table 3). The error bars are given at a $90\%$ confidence level.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1154_fig19.ps} \end{figure}$	Figure 10: EPIC spectra of the central source 1WGA J1713.4-3949 of the SNR RX J1713.7-3946 (MOS1 in black, MOS2 in red and pn in green). Best-fit obtained with a double blackbody model.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1154_fig20.eps} \end{figure}$	Figure 11: Optical image between 2300 and 3000 Å (Second Generation Digitized Sky Survey in red color at 450-600 THz) overlaid with the contour of the 2-10 keV X-ray image of SNR RX J1713.7-3946. The scaling is linear with the higher cut fixed at $5 \sigma$ of the mean optical brightness value.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1154_fig23.ps} \end{figure}$	Figure 14: Average CO spectra obtained towards the NW (continuous line) and towards the SW (dotted line) from the CfA CO survey (Dame et al. 2001). The SW emission is higher than the NW emission for LSR velocities between 0 and -10 km s^-1.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1154_fig24.ps} \end{figure}$	Figure 15: Kinetic energy of the explosion as a function of the SNR age for several solar masses of the supernova ejecta ( $M_{{\rm ej}} = 10, 15$ and $20 ~ {M}_{\odot}$ ) and different ambient medium densities ( $n_0 = 5 \times 10^{-3}, 1 \times 10^{-3}$ and $5 \times 10^{-4}$ cm^-3).
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