$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3530.f1.ps} \end{figure}$ Figure 1: Comparison of our best model of the X-ray surface brightness (dot-dashed ellipses) with the corresponding ROSAT image for the cluster A2597. The X-ray iso-contours are 0.5, 1, 3, 10 and 100 times the background; they were made after smoothing the original image with a Gaussian kernel of $\sigma = 3.2$ pixels.
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In the text

$\begin{figure} \par\psfig{file=3530.f2.ps,width=8cm,clip=} \end{figure}$ Figure 2: 3D deprojected gas (full lines) and dark matter (dashed lines) density profiles divided by the critical density of the Universe at the cluster redshift.
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In the text

$\begin{figure} \par\psfig{file=3530.f3.ps,width=8.8cm,clip} \end{figure}$ Figure 3: Synthetic cumulative dynamical mass profiles normalized to the corresponding total integrated cluster mass $M_{\rm Dyn}$ . The radial coordinate is normalized to the cluster r₂₀₀ radius.
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In the text

$\begin{figure} \par\psfig{file=3530.f7.ps,width=8.8cm,clip=} \end{figure}$ Figure 7: Synthetic 3D temperature profiles calculated from Eqs. (10) and (11) with the values of $\kappa$ given in Table 2. The temperature is normalized to the global cluster temperature and the radial coordinate is normalized to the cluster r₂₀₀ radius.
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In the text

$\begin{figure} \par\psfig{file=3530.f8.eps,width=12cm,height=7cm} %\end{figure}$ Figure 8: Re-projected emission weighted temperature deduced from our model. The projected radii s are normalized to the corresponding r_v = r₂₀₀ radii, and the temperatures are normalized to the observed isothermal temperatures.
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In the text

$\begin{figure} \par\psfig{figure=3530.f9.ps,angle=-90,width=8.8cm,clip=} \end{figure}$ Figure 9: Relation between L_X and T_X. The point at the lower left corner corresponds to the group HCG 62. The solid line shows the best fit (see text) and the dotted line is the fit found by Markevitch (1998).
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In the text

$\begin{figure} \par\psfig{figure=3530.f10.ps,height=6cm,width=8cm,clip=} \end{figure}$ Figure 10: Relation between the gas integrated specific entropy, $s_{\rm gas}$ and the gas mass. The best fit line is indicated (see text).
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In the text

$\begin{figure} \par\psfig{figure=3530.f11.ps,width=5.5cm,angle=-90,clip=} \end{figure}$ Figure 11: Relation between the gas integrated specific entropy and the mean gas temperature taken from the literature (see text). The point at the lower left corner corresponds to the group HCG 62.
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In the text

$\begin{figure} \par\psfig{figure=3530.f13.ps,width=8cm,height=6cm,clip=} \end{figure}$ Figure 13: Relation between the dark matter integrated specific entropy and mass. The best fit line is indicated (see text).
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In the text

$\begin{figure} \par\psfig{figure=3530.f14.ps,height=7cm,clip=} \end{figure}$ Figure 14: Relation between the dynamical mass and the potential energy. The solid line corresponds to the best fit to the data and the dashed line is the theoretical slope of I=5/3 defined by the relation $\ln(U_{\rm pot})-I\ \ln(M_{\rm dyn})={\rm const}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3530.f1.ps} \end{figure}$	Figure 1: Comparison of our best model of the X-ray surface brightness (dot-dashed ellipses) with the corresponding ROSAT image for the cluster A2597. The X-ray iso-contours are 0.5, 1, 3, 10 and 100 times the background; they were made after smoothing the original image with a Gaussian kernel of $\sigma = 3.2$ pixels.
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$\begin{figure} \par\psfig{file=3530.f2.ps,width=8cm,clip=} \end{figure}$	Figure 2: 3D deprojected gas (full lines) and dark matter (dashed lines) density profiles divided by the critical density of the Universe at the cluster redshift.
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$\begin{figure} \par\psfig{file=3530.f3.ps,width=8.8cm,clip} \end{figure}$	Figure 3: Synthetic cumulative dynamical mass profiles normalized to the corresponding total integrated cluster mass $M_{\rm Dyn}$ . The radial coordinate is normalized to the cluster r₂₀₀ radius.
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$\begin{figure} \par\psfig{file=3530.f4.ps,width=8.8cm,clip=} \end{figure}$	Figure 4: Correlation between the density profile parameters $a_{\rm eq}$ and $\nu$ .
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$\begin{figure} \par\psfig{file=3530.f5.ps,width=8.8cm,clip=} \end{figure}$	Figure 5: Correlation between the density profile parameters $\Sigma _0$ and $\nu$ .
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$\begin{figure} \par\psfig{file=3530.f6.ps,width=8.8cm,clip=} \end{figure}$	Figure 6: Correlation between the density profile parameters $\Sigma _0$ and $a_{\rm eq}$ .
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$\begin{figure} \par\psfig{file=3530.f7.ps,width=8.8cm,clip=} \end{figure}$	Figure 7: Synthetic 3D temperature profiles calculated from Eqs. (10) and (11) with the values of $\kappa$ given in Table 2. The temperature is normalized to the global cluster temperature and the radial coordinate is normalized to the cluster r₂₀₀ radius.
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$\begin{figure} \par\psfig{file=3530.f8.eps,width=12cm,height=7cm} %\end{figure}$	Figure 8: Re-projected emission weighted temperature deduced from our model. The projected radii s are normalized to the corresponding r_v = r₂₀₀ radii, and the temperatures are normalized to the observed isothermal temperatures.
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$\begin{figure} \par\psfig{figure=3530.f9.ps,angle=-90,width=8.8cm,clip=} \end{figure}$	Figure 9: Relation between L_X and T_X. The point at the lower left corner corresponds to the group HCG 62. The solid line shows the best fit (see text) and the dotted line is the fit found by Markevitch (1998).
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$\begin{figure} \par\psfig{figure=3530.f10.ps,height=6cm,width=8cm,clip=} \end{figure}$	Figure 10: Relation between the gas integrated specific entropy, $s_{\rm gas}$ and the gas mass. The best fit line is indicated (see text).
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$\begin{figure} \par\psfig{figure=3530.f11.ps,width=5.5cm,angle=-90,clip=} \end{figure}$	Figure 11: Relation between the gas integrated specific entropy and the mean gas temperature taken from the literature (see text). The point at the lower left corner corresponds to the group HCG 62.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3530.f12.ps} \end{figure}$	Figure 12: K₀ profiles based on density and temperature models.
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$\begin{figure} \par\psfig{figure=3530.f13.ps,width=8cm,height=6cm,clip=} \end{figure}$	Figure 13: Relation between the dark matter integrated specific entropy and mass. The best fit line is indicated (see text).
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$\begin{figure} \par\psfig{figure=3530.f14.ps,height=7cm,clip=} \end{figure}$	Figure 14: Relation between the dynamical mass and the potential energy. The solid line corresponds to the best fit to the data and the dashed line is the theoretical slope of I=5/3 defined by the relation $\ln(U_{\rm pot})-I\ \ln(M_{\rm dyn})={\rm const}$ .
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