All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0687fig1.ps}\end{figure}$ Figure 1: The predicted X-ray temperature function at redshifts z=0.05 (black), 0.33 (light grey) and 0.5 (dark grey) for a flat high density model (left; $\Omega _{\Lambda }=0.12$ ) and a concordance model (right; $\Omega _{\Lambda }=0.7$ ), both fitted to the local ( $z \sim 0.05$ ) temperature function.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0687fig2.ps}\end{figure}$ Figure 2: Count rate in PN ( top) and MOS ( bottom) cameras in the RX J1120.1 observation after selection for single pixel events above 10 keV. Typical rates $\sim$ 15 cts/50 s bin (PN) and $\sim$ 8 cts/100 s bin (MOS)
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In the text

$\begin{figure} \par {\includegraphics[width=7.3cm,clip]{0687fig3.ps} } \par \par\end{figure}$ Figure 3: Histogram of the count rate sequence for PN ( top) and MOS ( bottom) cameras in the RX J1120.1 observation after selection for single pixel events above 10 keV. The dashed lines indicate the upper and lower ( ${\pm } 3 \sigma$ ) bounds used for the Good Time Interval filtering.
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{0687fig4.ps} } \par \end{figure}$ Figure 4: Comparison of the relative scaling of particle (triangle) and proton (square) background rates ( after GTI filtering) in the eight cluster observations, with respect to the components of the background template files. Data averaged for all cameras in observation.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{0687fig5.ps} } \end{figure}$ Figure 5: Ratio of the surface brightness distributions in blank fields, showing proton contamination in RX J1701.3+6414 field.
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In the text

$\begin{figure} \par {\includegraphics[width=17.5cm]{0687f6.eps} }\end{figure}$ Figure 6: a) Central ${\sim } 18 \times 18$ arc-min of the RX J1120.1 field - smoothed by a $4'' \sigma$ Gaussian. The large circle represents the spectral extraction radius, and the smaller circles locate the point sources which were excised. Similar images for RX J1334.3 b), RX J0337.7 c) and RX J0505.3 d). The RX J1334.3 image $15\times 15$ arc-min; the RX J0337.7 and RX J0505.3 images are $14\times 14$ arc-min.
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In the text

$\begin{figure} \par {\includegraphics[width=17.5cm,clip]{0687fig7.ps} }\end{figure}$ Figure 7: a) Central MOS CCD image (10 arc-min) of the RX J0847.2 field - smoothed by a 4''Gaussian. The large circle represents the spectral extraction radius, and the smaller circles locate the point sources which were excised. Similar images for RX J1325.5 b), RX J1701.3 c) and RX J1354.2 d). A newly discovered candidate distant cluster (XMMU J084701.8+345117) is labeled to the upper right of RX J0847.2. The RX J1325.5 and RX J1325.0 Southern SHARC clusters fall in an observation centered on IRAS 13224-3809. The long steak connected to IRAS 13224-3809 comes from the "out-of-time" events collected during readout of the PN camera. In the RX J1701.3 field, the nearby Abell 2246 and QSO objects are labeled. The RX J1325.5 image is ${\sim } 18 \times 18$ arcmin; the RX J1701.3 and RX J1354.2 images are ${\sim } 14\times 14$ arcmin.
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In the text

$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig8.ps} }\end{figure}$ Figure 8: Spectral fit and residuals for RX J1120.1; black - PN, dark and light grey - MOS1 & 2 (double background subtraction).
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{0687fig9.ps} } \end{figure}$ Figure 9: The spatially resolved temperature profile of RX J1120.
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In the text

$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig10.ps} }\end{figure}$ Figure 10: Spectral fit and residuals for RX J1334.3; black - PN, dark & light gray - MOS1 & 2 (in-field background subtraction).
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In the text

$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig11.ps} }\end{figure}$ Figure 11: Spectral fit and residuals for RX J0337.7; black - PN, dark & light grey - MOS1 & 2.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{0687fig12.ps} \end{figure}$ Figure 12: Spectral fit and residuals for RX J0505.3; black - PN, dark & light grey - MOS.
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In the text

$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig13.ps} }\end{figure}$ Figure 13: Spectral fit and residuals for RX J0847.2 (MOS data only).
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In the text

$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig14.ps} }\end{figure}$ Figure 14: Spectral fit and residuals for RX J1325.5 (PN data only).
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In the text

$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig15.ps} } \par\end{figure}$ Figure 15: Spectral fit and residuals for RX J1701.3; black - PN, dark & light grey - MOS.
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In the text

$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig16.ps} } \end{figure}$ Figure 16: Spectral fit and residuals for RX J1354.2 black - PN, dark & light grey - MOS.
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In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{0687fig17.ps} }\end{figure}$ Figure 17: L_x-T_x relation for an EdS model (q₀=0.5) and H₀=50 km s^-1 Mpc^-1. The solid line is the best fit for our sample after cooling flow excision, the dotted line is the relation from Markevitch (1998) for low red-shift clusters.
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In the text

$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{0687fig18.ps} }\par\end{figure}$ Figure 18: L_x-T_x relation for H₀=70, $\Omega _{\Lambda }=0.7, \Omega _{\rm M}=0.3$ . The dotted horizontal lines are the CHANDRA sample reported by Vikhlinin et al. (2002), and the dashed diagonal line the Markevitch (1998) L_x-T_xrelation corrected to this cosmology. The solid crosses indicate the results from the clusters in our study, corrected for this cosmological model, and the diagonal solid line is the best fit for our data.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0687fig19a.ps}\hspace*{1.2... ...s}\hspace*{1.2cm} \includegraphics[width=8.1cm,clip]{0687fig19c.ps} \end{figure}$ Figure 19: Surface brightness distribution of clusters, compared with best $\beta$ -model fit (dotted line). Reading clockwise from top left: RX J1120.1, RX J1334.3, RX J0337.7 and RX J0505.3.
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In the text

$\begin{figure} \par\includegraphics[height=5.6cm,width=8.25cm,clip]{0687fig20a.p... ...5cm} \includegraphics[height=5.6cm,width=7.9cm,clip]{0687fig20c.ps} \end{figure}$ Figure 20: Surface brightness distribution of clusters, compared with best $\beta$ -model fit (dotted line). Reading clockwise from top left: RX J0847.2, RX J1325.5, RX J1701.1 and RX J1354.2.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0687fig1.ps}\end{figure}$	Figure 1: The predicted X-ray temperature function at redshifts z=0.05 (black), 0.33 (light grey) and 0.5 (dark grey) for a flat high density model (left; $\Omega _{\Lambda }=0.12$ ) and a concordance model (right; $\Omega _{\Lambda }=0.7$ ), both fitted to the local ( $z \sim 0.05$ ) temperature function.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0687fig2.ps}\end{figure}$	Figure 2: Count rate in PN ( top) and MOS ( bottom) cameras in the RX J1120.1 observation after selection for single pixel events above 10 keV. Typical rates $\sim$ 15 cts/50 s bin (PN) and $\sim$ 8 cts/100 s bin (MOS)
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$\begin{figure} \par {\includegraphics[width=7.3cm,clip]{0687fig3.ps} } \par \par\end{figure}$	Figure 3: Histogram of the count rate sequence for PN ( top) and MOS ( bottom) cameras in the RX J1120.1 observation after selection for single pixel events above 10 keV. The dashed lines indicate the upper and lower ( ${\pm } 3 \sigma$ ) bounds used for the Good Time Interval filtering.
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$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{0687fig4.ps} } \par \end{figure}$	Figure 4: Comparison of the relative scaling of particle (triangle) and proton (square) background rates ( after GTI filtering) in the eight cluster observations, with respect to the components of the background template files. Data averaged for all cameras in observation.
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{0687fig5.ps} } \end{figure}$	Figure 5: Ratio of the surface brightness distributions in blank fields, showing proton contamination in RX J1701.3+6414 field.
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$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig8.ps} }\end{figure}$	Figure 8: Spectral fit and residuals for RX J1120.1; black - PN, dark and light grey - MOS1 & 2 (double background subtraction).
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$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{0687fig9.ps} } \end{figure}$	Figure 9: The spatially resolved temperature profile of RX J1120.
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$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig10.ps} }\end{figure}$	Figure 10: Spectral fit and residuals for RX J1334.3; black - PN, dark & light gray - MOS1 & 2 (in-field background subtraction).
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$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig11.ps} }\end{figure}$	Figure 11: Spectral fit and residuals for RX J0337.7; black - PN, dark & light grey - MOS1 & 2.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{0687fig12.ps} \end{figure}$	Figure 12: Spectral fit and residuals for RX J0505.3; black - PN, dark & light grey - MOS.
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$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig13.ps} }\end{figure}$	Figure 13: Spectral fit and residuals for RX J0847.2 (MOS data only).
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$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig14.ps} }\end{figure}$	Figure 14: Spectral fit and residuals for RX J1325.5 (PN data only).
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$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig15.ps} } \par\end{figure}$	Figure 15: Spectral fit and residuals for RX J1701.3; black - PN, dark & light grey - MOS.
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$\begin{figure} \par {\includegraphics[angle=270,width=8.8cm,clip]{0687fig16.ps} } \end{figure}$	Figure 16: Spectral fit and residuals for RX J1354.2 black - PN, dark & light grey - MOS.
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$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{0687fig17.ps} }\end{figure}$	Figure 17: L_x-T_x relation for an EdS model (q₀=0.5) and H₀=50 km s^-1 Mpc^-1. The solid line is the best fit for our sample after cooling flow excision, the dotted line is the relation from Markevitch (1998) for low red-shift clusters.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0687fig19a.ps}\hspace{1.2... ...s}\hspace{1.2cm} \includegraphics[width=8.1cm,clip]{0687fig19c.ps} \end{figure}$	Figure 19: Surface brightness distribution of clusters, compared with best $\beta$ -model fit (dotted line). Reading clockwise from top left: RX J1120.1, RX J1334.3, RX J0337.7 and RX J0505.3.
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$\begin{figure} \par\includegraphics[height=5.6cm,width=8.25cm,clip]{0687fig20a.p... ...5cm} \includegraphics[height=5.6cm,width=7.9cm,clip]{0687fig20c.ps} \end{figure}$	Figure 20: Surface brightness distribution of clusters, compared with best $\beta$ -model fit (dotted line). Reading clockwise from top left: RX J0847.2, RX J1325.5, RX J1701.1 and RX J1354.2.
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