All Figures

$\begin{figure} \par\includegraphics[width=16.45cm,clip]{5681fig1.eps} \end{figure}$ Figure 1: Dust map (E(B-V) map from Schlegel et al. (1998) in logarithmic grey scale) superposed with all known clusters and groups found in NED with $\vert b\vert < 20^{\circ }$ and $20^{\circ } < l < 200^{\circ }$ . Cl 2334+48 is emphasised with a larger symbol near $l = 110^{\circ }$ , $b = -12^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5681fig2.eps} \end{figure}$ Figure 2: Top: EPIC MOS1+MOS2 image of Cl 2334+48 in the 0.5-8.0 keV band. The lines are adaptively smoothed contours in logarithmic scales. Bottom: the smoothed X-ray contours superposed on the $i^\prime$ -band image. The circles indicate the identified galaxies inside a region of radius 270 h₇₀^-1 kpc. Squares mark the next three brightest galaxies after the first-ranked galaxy (see Sect. 6 and Fig. 10). An arc-like feature is indicated with an arrow (see Sect. 6).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5681fig3.eps} \end{figure}$ Figure 3: X-ray surface brightness fitted with a $\beta$ -model and Sérsic law (see text for details).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{5681fig4.ps} \end{figure}$ Figure 4: EPIC spectra with the best-fit model (solid lines; see Table 2).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5681fig5.ps} \end{figure}$ Figure 5: Radial temperature profile (see Sect. 4.2.1). The dashed line represents the mean temperature ( $\it kT$ = 4.92 keV; dotted line for their limits) derived from the spectrum extract within $R < 65\hbox {$^{\prime \prime }$ }$ . Error bars are at the 90% confidence level.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5681fig6.eps} \end{figure}$ Figure 6: Top: gas and dynamical (total) mass cumulative profiles. The vertical lines indicate the r₂₅₀₀ and r₅₀₀₀ radii (see text). Bottom: the gas mass fraction (baryon fraction minus the contribution from galaxies).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5681fig7.eps} \end{figure}$ Figure 7: Total mass density profile for both $\beta$ -model and Sérsic law. The long-dashed line shows $\rho$ $\propto$ r^-1 as a reference.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{5681fig8.eps} \end{figure}$ Figure 8: The optical spectrum of the central galaxy, de-redshifted and smoothed with a boxcar filter.
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{5681fig9.ps} \end{figure}$ Figure 9: Density of galaxies with 16.3 < $m_{i^\prime }$ < 21 as a function of the distance from the central galaxy in steps of 33 $\hbox {$^{\prime \prime }$ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5681fg10.ps} \end{figure}$ Figure 10: Colour-magnitude diagram in the $g^{\prime }$ and $i^\prime$ bands inside a circle of radius 65 $^{\prime \prime }$ , centred on the brightest cluster galaxy. The next three brightest galaxies after the first-ranked galaxy of the cluster are marked with squares (see Sect. 6).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5681fg11.ps} \end{figure}$ Figure 11: Surface brightness of the central galaxy in the $i^\prime$ band. The solid line represents a r^1/4 (de Vaucouleurs) profile. The size of the symbols represents upper limits of the estimated errors of $\mu _{i^{\prime }}$ .
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In the text

$\begin{figure} \par\includegraphics[width=16.45cm,clip]{5681fig1.eps} \end{figure}$	Figure 1: Dust map (E(B-V) map from Schlegel et al. (1998) in logarithmic grey scale) superposed with all known clusters and groups found in NED with $\vert b\vert < 20^{\circ }$ and $20^{\circ } < l < 200^{\circ }$ . Cl 2334+48 is emphasised with a larger symbol near $l = 110^{\circ }$ , $b = -12^{\circ }$ .
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5681fig3.eps} \end{figure}$	Figure 3: X-ray surface brightness fitted with a $\beta$ -model and Sérsic law (see text for details).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{5681fig4.ps} \end{figure}$	Figure 4: EPIC spectra with the best-fit model (solid lines; see Table 2).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5681fig5.ps} \end{figure}$	Figure 5: Radial temperature profile (see Sect. 4.2.1). The dashed line represents the mean temperature ( $\it kT$ = 4.92 keV; dotted line for their limits) derived from the spectrum extract within $R < 65\hbox {$^{\prime \prime }$ }$ . Error bars are at the 90% confidence level.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5681fig6.eps} \end{figure}$	Figure 6: Top: gas and dynamical (total) mass cumulative profiles. The vertical lines indicate the r₂₅₀₀ and r₅₀₀₀ radii (see text). Bottom: the gas mass fraction (baryon fraction minus the contribution from galaxies).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5681fig7.eps} \end{figure}$	Figure 7: Total mass density profile for both $\beta$ -model and Sérsic law. The long-dashed line shows $\rho$ $\propto$ r^-1 as a reference.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{5681fig8.eps} \end{figure}$	Figure 8: The optical spectrum of the central galaxy, de-redshifted and smoothed with a boxcar filter.
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$\begin{figure} \par\includegraphics[width=7.85cm,clip]{5681fig9.ps} \end{figure}$	Figure 9: Density of galaxies with 16.3 < $m_{i^\prime }$ < 21 as a function of the distance from the central galaxy in steps of 33 $\hbox {$^{\prime \prime }$ }$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5681fg10.ps} \end{figure}$	Figure 10: Colour-magnitude diagram in the $g^{\prime }$ and $i^\prime$ bands inside a circle of radius 65 $^{\prime \prime }$ , centred on the brightest cluster galaxy. The next three brightest galaxies after the first-ranked galaxy of the cluster are marked with squares (see Sect. 6).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5681fg11.ps} \end{figure}$	Figure 11: Surface brightness of the central galaxy in the $i^\prime$ band. The solid line represents a r^1/4 (de Vaucouleurs) profile. The size of the symbols represents upper limits of the estimated errors of $\mu _{i^{\prime }}$ .
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