All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{x5pnS_vnei_vrayCMJN.eps} \end{figure}$ Figure 1: EPIC-pn spectra of SN 1987 A from Jan. 2000, April 2001 and May 2003 (in increasing intensity). The histograms show the best fit model A as defined in Table 2 and parameters listed in Tables 3 and 4.
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In the text

$\begin{figure} \includegraphics[width=12cm,clip=]{vnei_vray_PN2MOSCMJN.eps} \end{figure}$ Figure 2: EPIC-MOS spectra of SN 1987 A from satellite revolution 626. The histograms show the prediction of model A with the best-fit parameter values of the EPIC-pn spectrum except the normalization (a constant scaling factor of 0.98 and 0.99 for MOS1 and MOS2, respectively).
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In the text

$\begin{figure} \includegraphics[width=12cm,clip=]{vnei_vray_PN2RGSCMJN.eps} \end{figure}$ Figure 3: RGS spectra of SN 1987 A from satellite revolution 626. The model is as for Fig. 2 with scaling factors 1.01 and 0.98 for RGS1 and RGS2, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{SN1987A_lc_lin_log.eps} \end{figure}$ Figure 4: X-ray light curve of SN 1987 A in the 0.5-2.0 keV band. Chandra ACIS-S fluxes were corrected for pile-up losses as described in Sect. 4. The insert shows the light curve in logarithmic intensity scale together with the model described in Sect. 4.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{sn87a_model1CMJN.eps} \end{figure}$ Figure 5: Sketch used to model the matter distribution around SN 1987 A. The matter is arranged in a circular torus of radius $r\sb {\rm c}$ ; lines of constant density form circles which build up the torus. For torus circles up to radius $r\sb {\rm t}$ the distribution follows a Gaussian which has its peak at $r\sb {\rm c}$ and falls off with increasing $\Delta r$ . Outside of $r\sb {\rm t}$ the distribution is roughly exponential which peaks at $r\sb {\rm t}$ and decreases with increasing $\Delta r$ . For each location in space (r, $\Theta$ , $\phi$ ) the density is defined according to this scheme (no dependence on $\phi$ ). The big circle represents the radius of the forward shock wave at day 7000, which has just passed the torus center.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{x5pnS_vnei_vrayCMJN.eps} \end{figure}$	Figure 1: EPIC-pn spectra of SN 1987 A from Jan. 2000, April 2001 and May 2003 (in increasing intensity). The histograms show the best fit model A as defined in Table 2 and parameters listed in Tables 3 and 4.
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$\begin{figure} \includegraphics[width=12cm,clip=]{vnei_vray_PN2MOSCMJN.eps} \end{figure}$	Figure 2: EPIC-MOS spectra of SN 1987 A from satellite revolution 626. The histograms show the prediction of model A with the best-fit parameter values of the EPIC-pn spectrum except the normalization (a constant scaling factor of 0.98 and 0.99 for MOS1 and MOS2, respectively).
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$\begin{figure} \includegraphics[width=12cm,clip=]{vnei_vray_PN2RGSCMJN.eps} \end{figure}$	Figure 3: RGS spectra of SN 1987 A from satellite revolution 626. The model is as for Fig. 2 with scaling factors 1.01 and 0.98 for RGS1 and RGS2, respectively.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{SN1987A_lc_lin_log.eps} \end{figure}$	Figure 4: X-ray light curve of SN 1987 A in the 0.5-2.0 keV band. Chandra ACIS-S fluxes were corrected for pile-up losses as described in Sect. 4. The insert shows the light curve in logarithmic intensity scale together with the model described in Sect. 4.
Open with DEXTER