Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{MS2856fig1.eps}\par\end{figure}$ Figure 1: Temperature profiles. The temperatures have been normalised to the spectroscopic temperature measured in 0.1<r<0.5 R₂₀₀region; the radius has been scaled to R₂₀₀. The profiles have been corrected for PSF and projection effects (see Paper I for details).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{MS2856fig2.ps} \par\end{figure}$ Figure 2: The M-T relation at $\delta =2500$ as seen by XMM-Newton from the observation of 6 hot (kT>3.5 keV), relaxed clusters. Filled squares show the XMM-Newton data points; the full line shows the best fitting power law. The data on 4 published Chandra clusters (triangles) have been added to the fit but due to their larger uncertainties, they do not change the parameters of the fit to the XMM-Newton data only (see text). The dashed black line is the prediction from adiabatic numerical simulations (Evrard et al. 1996).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{MS2856fig3.ps} % \par\end{figure}$ Figure 3: The M-T relation as seen by XMM-Newton from a sample of 10 clusters covering a temperature range from 2 to 9 keV. From top to bottom and left to right, the M-T relation is given at the density contrasts $\delta$ of 200, 500, 1000 and 2500 with respect to the critical density of the Universe. Measurements are plotted with error bars. In each panel, the best fit for the whole sample is overplotted as a solid line, and the best fit for the hot cluster subsample is plotted as a dotted line. The predicted relation from adiabatic numerical simulations (Evrard et al. 1996) is overplotted as a dashed line. The long-dashed line (panels $\delta =500$ and $\delta =2500$ ) is the relation derived from a numerical simulation including radiative cooling, star formation and SN feedback (Borgani et al. 2004).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{MS2856fig4.eps} \par\end{figure}$ Figure 4: The normalisation of the $M_\delta$ -T relation at $T=5~\rm keV$ for various $\delta$ . The results of theoretical works (see Table 3 for references) are compared to the values derived in the present work (PW) .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{MS2856fig1.eps}\par\end{figure}$	Figure 1: Temperature profiles. The temperatures have been normalised to the spectroscopic temperature measured in 0.1<r<0.5 R₂₀₀region; the radius has been scaled to R₂₀₀. The profiles have been corrected for PSF and projection effects (see Paper I for details).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{MS2856fig4.eps} \par\end{figure}$	Figure 4: The normalisation of the $M_\delta$ -T relation at $T=5~\rm keV$ for various $\delta$ . The results of theoretical works (see Table 3 for references) are compared to the values derived in the present work (PW) .
Open with DEXTER