All Tables

Table 1: The CXB components used in the fitting of the A3128 spectra. The power-law photon index is $\Gamma =1.41$ . The unabsorbed fluxes are determined in the 0.3-10.0 keV band.
Table 2: Fit results for the spectra extracted from the SW X-ray peak, from the apparent "tail'' of the NE peak toward SW, and from the NE X-ray peak. The spectra extracted from the SW peak and from the "tail'' region were fitted with a thermal model with the $N_{{\rm H}}$ fixed to the Galactic value ( $N_{{\rm H}}=1.47\times 10^{20}$ cm^-2, Dickey & Lockman 1990). The NE X-ray peak was fitted with two thermal models: one for the emission from A3128 in the foreground and one for the background cluster. In this fit the redshift, temperature, and the Fe abundance of the foreground cluster were fixed to the best fit values from the "tail'' region. The reported best fit parameter of the NE peak describe the properties of the background cluster. The temperature is given in keV, the emission measure Y is given in units of 10⁶⁵ cm^-3 and the Fe abundance is given with respect to the proto-solar values of Lodders (2003).
Table 3: Radial profiles determined for the SW X-ray peak. The temperature is given in keV, the emission measure Y is given in units of 10⁶⁵ cm^-3, and the Fe abundance is given with respect to the proto-solar values of Lodders (2003).
Table 4: Radial profiles determined for the NE X-ray peak. The metallicity and the temperature of the foreground cluster were fixed to 0.49 solar and 3.5 keV, respectively. The emission measure Y is given in units of 10⁶⁵ cm^-3 and the temperature is given in keV. The Fe abundance is given with respect to the proto-solar values of Lodders (2003). The f_z=0.44 / f_z=0.06 indicates the ratio of the fluxes from the background cluster and A3128 in the given extraction region. The superscript "f'' indicates that the parameter value was fixed during the fitting.
Table 5: The best fit values determined for the X-ray bright low entropy region and for the region at the centre of the galaxy distribution. The emission measure Y_S per square arcminute is given in units of 10⁶⁴ cm^-3 arcmin^-2 and the temperatures are in keV. The Fe abundance is given with respect to the proto-solar values of Lodders (2003). The entropy s is given in keV cm² and the pressure P is given in 10^-12 dyne cm^-2.