All Figures

$\begin{figure} \par\includegraphics[width=4cm,angle=-90]{Figs/9168fig1.eps}\incl... ...fig11.eps}\includegraphics[width=4cm,angle=-90]{Figs/9168fig12.eps} \end{figure}$ Figure 1: Comparison between observation background and Lumb background for MOS1 ( left panel), MOS2 ( middle panel) and PN ( right panel). The black points correspond to the observation data, the red points to Lumb scaled background and the green points represent the residual.
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In the text

$\begin{figure} \includegraphics[angle=90,width=12cm,clip]{Figs/9168fig13.ps} \end{figure}$ Figure 2: Surface brightness profile (black points) of our clusters A496, A2667, A2050, A2631 and A1689. $\beta$ -model fits are represented by red continuous lines and the Sérsic fits are represented by blue dashed lines. The vertical dashed lines represent r₅₀₀. For A496 the r₅₀₀ is beyond the range of the X-axis.
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In the text

$\begin{figure} \par\includegraphics[width=4.2cm,angle=90]{Figs/9168fig14.ps}\par... ...17.ps}\par\includegraphics[width=4.2cm,angle=90]{Figs/9168fig18.ps} \end{figure}$ Figure 3: Temperature profile for A469, A1689, A2667, A2050 and A2667. For A496, A1689 and A2667 2D analytical fits given by Eq. (9) are represented by the red solid lines, the blue dot-dashed lines represent the computed deprojected temperature profile given by Eq. (10) and the mean temperatures are represented by the horizontal dashed lines. For A1689, A2050 and A2631 the mean temperatures are represented by the horizontal dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{Figs/9168fig19.ps} \end{figure}$ Figure 4: Temperature maps, substructure maps and optical image overlaid with X-ray contours for A496, A1689, A2050, A2631 and A2667, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,angle=90]{Figs/9168fig20.ps} \end{figure}$ Figure 5: Color-magnitude diagram of galaxies within r₅₀₀ in the field of view of A2050. The near-horizontal solid line indicates the separation between cluster and background galaxies. The equation of the solid line is $g^{\prime }-i^{\prime }=2.37{-}0.055i^{\prime }$ . The vertical dashed line indicates the $i^{\prime }$ magnitude limit.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm]{Figs/9168fig21.ps} \end{figure}$ Figure 6: Number of galaxies per area of each annulus as a function of r₅₀₀ for A1689. The background can be determined beyond R= 7 r₅₀₀.
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In the text

$\begin{figure} \par\includegraphics[width=4.2cm,angle=90]{Figs/9168fig22.ps}\par... ...24.ps}\par\includegraphics[width=4.2cm,angle=90]{Figs/9168fig25.ps} \end{figure}$ Figure 7: Luminosity function for clusters for which we have optical data: A496, A1689, A2050 and A2631, respectively. For A496 the double Schechter fit (given by Eq. (14)) is represented by the solid line and the single Schechter fit (given by Eq. (12)) is represented by the dotted line. For all other clusters we present only the single Schechter fit.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=90]{Figs/9168fig26.ps} \end{figure}$ Figure 8: $M_{\rm ICL+star}/M_{\rm gas}$ as a function of temperature for A496, A1689, A2050, A2631 and A2667 (red points). Our best fit (Eq. (28)) is represented by the solid line. Black points were obtained from Lin et al. (2003) and the blue dot-dashed line was their best fit ( $M_{\rm star}/M_{\rm gas} \propto kT^{0.23}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,angle=90]{Figs/9168fig27.ps} \end{figure}$ Figure 9: Gas and total stellar fraction as a function of cluster temperature. The black points represent the gas fraction while the red ones are the stellar fraction. For the stellar fraction we used both stars in galaxies and the ICL contribution.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,angle=-90]{Figs/9168fig1.eps}\incl... ...fig11.eps}\includegraphics[width=4cm,angle=-90]{Figs/9168fig12.eps} \end{figure}$	Figure 1: Comparison between observation background and Lumb background for MOS1 ( left panel), MOS2 ( middle panel) and PN ( right panel). The black points correspond to the observation data, the red points to Lumb scaled background and the green points represent the residual.
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$\begin{figure} \includegraphics[angle=90,width=12cm,clip]{Figs/9168fig13.ps} \end{figure}$	Figure 2: Surface brightness profile (black points) of our clusters A496, A2667, A2050, A2631 and A1689. $\beta$ -model fits are represented by red continuous lines and the Sérsic fits are represented by blue dashed lines. The vertical dashed lines represent r₅₀₀. For A496 the r₅₀₀ is beyond the range of the X-axis.
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$\begin{figure} \par\includegraphics[width=11cm,clip]{Figs/9168fig19.ps} \end{figure}$	Figure 4: Temperature maps, substructure maps and optical image overlaid with X-ray contours for A496, A1689, A2050, A2631 and A2667, respectively.
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$\begin{figure} \par\includegraphics[width=5cm,angle=90]{Figs/9168fig20.ps} \end{figure}$	Figure 5: Color-magnitude diagram of galaxies within r₅₀₀ in the field of view of A2050. The near-horizontal solid line indicates the separation between cluster and background galaxies. The equation of the solid line is $g^{\prime }-i^{\prime }=2.37{-}0.055i^{\prime }$ . The vertical dashed line indicates the $i^{\prime }$ magnitude limit.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm]{Figs/9168fig21.ps} \end{figure}$	Figure 6: Number of galaxies per area of each annulus as a function of r₅₀₀ for A1689. The background can be determined beyond R= 7 r₅₀₀.
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$\begin{figure} \par\includegraphics[width=4.2cm,angle=90]{Figs/9168fig22.ps}\par... ...24.ps}\par\includegraphics[width=4.2cm,angle=90]{Figs/9168fig25.ps} \end{figure}$	Figure 7: Luminosity function for clusters for which we have optical data: A496, A1689, A2050 and A2631, respectively. For A496 the double Schechter fit (given by Eq. (14)) is represented by the solid line and the single Schechter fit (given by Eq. (12)) is represented by the dotted line. For all other clusters we present only the single Schechter fit.
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$\begin{figure} \par\includegraphics[width=8cm,angle=90]{Figs/9168fig26.ps} \end{figure}$	Figure 8: $M_{\rm ICL+star}/M_{\rm gas}$ as a function of temperature for A496, A1689, A2050, A2631 and A2667 (red points). Our best fit (Eq. (28)) is represented by the solid line. Black points were obtained from Lin et al. (2003) and the blue dot-dashed line was their best fit ( $M_{\rm star}/M_{\rm gas} \propto kT^{0.23}$ ).
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$\begin{figure} \par\includegraphics[width=8.2cm,angle=90]{Figs/9168fig27.ps} \end{figure}$	Figure 9: Gas and total stellar fraction as a function of cluster temperature. The black points represent the gas fraction while the red ones are the stellar fraction. For the stellar fraction we used both stars in galaxies and the ICL contribution.
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