2003A&A...407...41C

We present the results from XMM-Newton observations of the cluster of galaxies PKS 0745-191. The spatially resolved spectra from the European Photon Imaging Cameras (both EPN and EMOS) can be fitted with a single temperature thermal plasma model when the interstellar column density is closer to the lower limit of the range allowed by observations. Alternatively, a two-component model can be fitted to the spectra from the inner region for slightly higher values of N_H. The temperature profile shows a drop in the center of the cluster, from about 8keV at radii larger than ∼350kpc to about 4keV at the center, indicating that the gas in the central region is cooling. The total cooling flow rate inferred from the spectral data is only 364⁺⁹⁷_–94M_☉/yr, however, much smaller than the previously obtained value. The metal abundance is found to decrease from 0.5 in solar units at the center to about 0.2 at a radius of ∼300kpc. Deprojected spectra are also presented, which show a result similar to the projected spectra. The location of the X-ray emission peak is also the site of extended radio emission. Inspection of the higher resolution Chandra image of the cluster shows enhanced X-ray emission about 3'' west of the center where also the radio emission is elongated. We explore possible implications on the interaction between the radio lobes and the intracluster plasma. Assuming that the gas is in hydrostatic equilibrium with the cluster potential, we find a total mass of about 1.18±0.04x10¹³M_☉ within the critical radius of the observed gravitational arc, which is a factor ∼2 lower, however, than that from optical lensing. We also calculated the gas mass fraction profile up to 0.63r_vir and obtained a mean gas mass fraction f_gas=0.22±0.02.