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$\begin{figure} \par\includegraphics[width=7cm,clip]{0122f1.eps} % \end{figure}$ Figure 1: Suzaku XIS-0 image of RX J1347.5-1145 in the 0.5-10 keV band. The spectral integration regions for the cluster and the background are indicated with the solid and dashed circles, respectively. The two corners of the CCD chip illuminated by ⁵⁵Fe calibration sources are excluded from the image.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8cm,clip]{0122f2a.eps} \includegraphics[angle=-90,width=8cm,clip]{0122f2b.eps} } \end{figure}$ Figure 2: a) Observed XIS spectra ( $r<5\hbox {$^\prime $ }$ ). The spectra taken by four sensors, XIS-0 (black), 1 (red), 2 (green), and 3 (blue), are shown separately. The solid lines in the upper panel show the best-fitting single-temperature APEC thermal plasma model simultaneously fit to all of the sensors, convolved with the telescope and the detector response functions. In the bottom panel the residuals of the fit in units of the number of standard deviations are shown. b) Blow-up of the XIS-0 spectrum in the 4-5.5 keV band. The single-temperature model fails to fit the He-like Fe K $\alpha$ line.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8cm,clip]{0122f3a.eps} \includegraphics[angle=-90,width=8cm,clip]{0122f3b.eps} } \end{figure}$ Figure 3: a) Observed XIS spectra in the 4-5.5 keV band. The spectra taken by four sensors, XIS-0 (black), 1 (red), 2 (green), and 3 (blue), are shown separately. The solid lines in the upper panels are the best-fitting continuum plus two Gaussian models. In the bottom panel the residuals of the fit in units of the number of standard deviations are shown. b) Line ratio (He-like Fe K $\alpha$ )/(H-like Fe K $\alpha$ ) as a function of temperature, calculated from the APEC model. The horizontal dashed line and the dotted lines show the best-fitting line ratio and the 90% confidence interval, respectively.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[angle=-90,width=7.5cm,clip]{0122f4a.eps} \includegraphics[angle=-90,width=7.5cm,clip]{0122f4b.eps} } \end{figure}$ Figure 4: a) Two-temperature APEC model fit to the observed XIS spectra. The spectra taken by four sensors, XIS-0 (black), 1 (red), 2 (green), and 3 (blue), are shown separately. The solid lines in the upper panel show the sum of two APEC models with different temperatures, while the dashed lines show the low-temperature (upper curves) and high-temperature (lower curves) components separately, convolved with the telescope and the detector response functions. In the bottom panel the residuals of the fit in units of the number of standard deviations are shown. b) Blow-up of the XIS spectra in the 4-5.5 keV band. The two-temperature model fits both the He-like and H-like Fe K $\alpha$ lines adequately.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.5cm,clip]{0122f5a.eps}\includegraphics[angle=-90,width=7.5cm,clip]{0122f5b.eps} } \end{figure}$ Figure 5: Observed PIN spectra during two observing periods of RX J1347.5-1145. a) Seq: 801013010; and b) Seq: 801013020.In each panel Data, NXB, and (Data-NXB) are shown with the black crosses, red crosses, and green circles, respectively.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.5cm,clip]{0122f6a.eps} \includegraphics[angle=-90,width=7.5cm,clip]{0122f6b.eps} } \end{figure}$ Figure 6: Observed light curves of the PIN 12-40 keV count rates during two observing periods. a) Seq: 801013010; and b) Seq: 801013020. In the upper panels, the Data and NXB rates are shown by black and red crosses, respectively. In the bottom panels, (Data-NXB) is shown by the green circles. The error bars show the 1 $\sigma$ statistical errors.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0122f7.eps}\end{figure}$ Figure 7: Observed PIN spectrum minus the nominal NXB model (Data-NXB; black), the simulated CXB model (red), and the point source contribution estimated from the XMM-Newton observations of the same field (green).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0122f8.eps}\end{figure}$ Figure 8: Observed PIN spectrum with the background model subtracted (Data-NXB-CXB; the crosses) in the 12-60 keV band. The error bars indicate only the statistical errors. The histogram shows the best-fit APEC thermal plasma model. The bottom panel shows the residuals in units of the number of standard deviations.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7cm,clip]{0122f9a.eps}... ...e*{2mm} \includegraphics[angle=-90,width=7cm,clip]{0122f9b.eps} } \end{figure}$ Figure 9: a) Chandra ACIS-I image in the 0.5-7 keV band. The solid lines show the NW and SE regions. The radius of the circle is 5 $^\prime$ . b) The surface brightness profiles of the position angle $0^{\circ }$ - $360^{\circ }$ (black), NW: $-90^{\circ }$ - $180^{\circ }$ (red), and SE: $180^{\circ }$ - $270^{\circ }$ (green). The black line shows the best-fit double $\beta$ -model for the position angle of $0^{\circ }$ - $360^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0122f10a.eps} \includegraphics[angle=-90,width=7.5cm,clip]{0122f10b.eps}\end{figure}$ Figure 10: a) Projected (crosses) and deprojected (circles) temperature profiles measured from the Chandra data in the NW region. b) Projected metal abundance profile (crosses). The horizontal dashed and dotted lines show the best-fit constant abundance and the corresponding 90% confidence interval obtained from the deprojection analysis, respectively. We assume that the metal abundance is constant over all radial bins throughout this paper.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0122f11a.eps} \includegraphics[angle=-90,width=7.5cm,clip]{0122f11b.eps}\end{figure}$ Figure 11: a) 6APEC $\times$ PLABS( $\alpha =0.02$ ) + APEC model, fit simultaneously to the observed XIS (0.5-10 keV) and PIN (12-60 keV) spectra. The spectra taken by four sensors, XIS-0 (black), 1 (red), 2 (green), and 3 (blue), are shown separately. The black and red lines show the ambient component (6APEC $\times$ PLABS) and the excess hot component described by an additional APEC model, respectively, convolved with the telescope and the detector response functions. In the bottom panel the residuals of the fit in units of the number of standard deviations are shown. We have used the nominal NXB model for the background of the PIN data (see Sect. 4.1). b) same as a), but for the unfolded XIS-0 and PIN spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0122f12a.eps} \includegraphics[angle=-90,width=7.5cm,clip]{0122f12b.eps}\end{figure}$ Figure 12: a) 6APEC $\times$ PLABS( $\alpha =0.02$ ) (thermal model for the ambient gas) + PL model (non-thermal model for the hot gas), fit simultaneously to the observed XIS (0.5-10 keV) and PIN (12-60 keV) spectra. The spectra taken by four sensors, XIS-0 (black), 1 (red), 2 (green), and 3 (blue), are shown separately. The black and red lines show the ambient component (6APEC $\times$ PLABS) and the excess hot component described by a non-thermal power-law model, respectively, convolved with the telescope and the detector response functions. In the bottom panel the residuals of the fit in units of the number of standard deviations are shown. We have used the nominal NXB model for the background of the PIN data (see Sect. 4.1). b) same as a), but for the unfolded XIS-0 and PIN spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{0122fa1.eps}\end{figure}$ Figure A.1: Suzaku/XIS+ Chandra/ACIS-I spectra of RX J1347.5-1145 ( $r<5\hbox {$^\prime $ }$ ) simultaneously fitted with the APEC $\times$ PLABS model.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0122f1.eps} % \end{figure}$	Figure 1: Suzaku XIS-0 image of RX J1347.5-1145 in the 0.5-10 keV band. The spectral integration regions for the cluster and the background are indicated with the solid and dashed circles, respectively. The two corners of the CCD chip illuminated by ⁵⁵Fe calibration sources are excluded from the image.
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.5cm,clip]{0122f5a.eps}\includegraphics[angle=-90,width=7.5cm,clip]{0122f5b.eps} } \end{figure}$	Figure 5: Observed PIN spectra during two observing periods of RX J1347.5-1145. a) Seq: 801013010; and b) Seq: 801013020.In each panel Data, NXB, and (Data-NXB) are shown with the black crosses, red crosses, and green circles, respectively.
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.5cm,clip]{0122f6a.eps} \includegraphics[angle=-90,width=7.5cm,clip]{0122f6b.eps} } \end{figure}$	Figure 6: Observed light curves of the PIN 12-40 keV count rates during two observing periods. a) Seq: 801013010; and b) Seq: 801013020. In the upper panels, the Data and NXB rates are shown by black and red crosses, respectively. In the bottom panels, (Data-NXB) is shown by the green circles. The error bars show the 1 $\sigma$ statistical errors.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0122f7.eps}\end{figure}$	Figure 7: Observed PIN spectrum minus the nominal NXB model (Data-NXB; black), the simulated CXB model (red), and the point source contribution estimated from the XMM-Newton observations of the same field (green).
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0122f8.eps}\end{figure}$	Figure 8: Observed PIN spectrum with the background model subtracted (Data-NXB-CXB; the crosses) in the 12-60 keV band. The error bars indicate only the statistical errors. The histogram shows the best-fit APEC thermal plasma model. The bottom panel shows the residuals in units of the number of standard deviations.
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{0122fa1.eps}\end{figure}$	Figure A.1: Suzaku/XIS+ Chandra/ACIS-I spectra of RX J1347.5-1145 ( $r<5\hbox {$^\prime $ }$ ) simultaneously fitted with the APEC $\times$ PLABS model.
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