All Tables

Table 1: Best-fit results of the spectral and spatial analysis of the sample of galaxy clusters at redshift >0.4 and derived quantities at an overdensity corresponding to $\Delta _z=500$ in a Einstein-de Sitter universe. A Hubble constant of 70 km s^-1 Mpc^-1 in a flat universe with $\Omega _{\rm m}$ equals to 0.3 is assumed. Note: (i) RX J1347-1145 has a clear hot enhancement to the South-East of the main X-ray emission. A sector with position angle $90^{\circ }{-}180^{\circ }$ and centered on the X-ray peak has been masked in accordance with the analysis presented in Allen et al. (2002). (ii) In 3C 295, the central active galactic nucleus and regions of enhanced emission associated to the radio lobes have been masked (see Allen et al. 2001a). (iii) MS1054-0321 presents significant substructure (e.g. Jeltema et al. 2001). The temperature and the best-fit of the surface brightness profile are estimated from the main body of the cluster once a circular region centered at (RA, Dec; 2000) = $(10^{\rm h} 56^{\rm m} 55\hbox {$^{\prime \prime }$ }7,-3^{\circ } 37' 37'')$ and with radius of 36 arcsec is masked.
Table 2: Mean, median and dispersion values for the best-fit parameters $r_{\rm c}$ and $\beta$ estimated for objects in the chosen redshift bins.
Table 3: Best-fit results on the scaling relations corrected by the cosmological factor E_z(dashed and dotted lines in the plots; see Eq. (5)). The temperature, $T_{\rm gas, 6}$ , is in unit of 6 keV; the luminosity, $L_{\rm bol, 44}$ , in 10⁴⁴ h₇₀^-2 erg s^-1; the total mass, $M_{\rm tot, 14}$ , in $10^{14}~ h_{70}^{-1}~ M_{\odot}$ ; the gas mass, $M_{\rm gas, 13}$ , in $10^{13}~ h_{70}^{-5/2} ~M_{\odot}$ . When the slope A is fixed, we estimate the error-weighted mean of $(\log Y -A \log X)$ and evaluate the error after resampling Y and Xby 1000 times according to their uncertainties. The scatter on Y is measured as $\left[ \sum_{j=1,N} \left(\log Y_j -\alpha -A \log X_j \right)^2 /N \right]^{1/2}$ . Note that the scatter along the X-axis can be estimated as $\sigma_{\log X} = \sigma_{\log Y} / A$ .
Table 4: The best-fit values of the evolution parameter B, B_z (see Eqs. (6) and (7) and comments in Sect. 4) are obtained by comparing to the local best-fit results, indicated in the second column and discussed in the text, the 28, 16 and 11 clusters with redshift larger than 0.4, 0.6 and 0.8, respectively. The case of no evolution corresponds to a value of B_z equal to 0. The L-T relation has been studied also not including the correction by E_z. This relation is then expected to be proportional to E_z and B should be measured in the range 0.6-0.9 in the adopted cosmology.