HIGH RESOLUTION XMM-NEWTON SPECTROSCOPY OF THE COOLING FLOW CLUSTER ABELL 3112

We examine high signal to noise XMM-Newton EPIC and RGS observations to determine the physical characteristics of the gas in the cool core and outskirts of the nearby rich cluster A3112. The XMM-ESAS data reduction and background modeling methods were used to analyze the XMMNewton EPIC data. From the EPIC data we nd that the iron and silicon abundance gradients show signicant increase towards the center of the cluster while the oxygen abundance prole is centrally peaked but has a shallower distribution than that of iron. The X-ray mass modeling is based on the temperature and deprojected density distributions of the intra-cluster medium determined from EPIC observations. The total mass of A3112 obeys the M T scaling relations found using XMM-Newton and Chandra observations of massive clusters at r500. The gas mass fraction fgas = 0:149 +0:036 0:032 at r500, is consistent with the 7-year WMAP results. The comparisons of line uxes and ux limits on the Fe XVII and Fe XVIII lines obtained from high resolution RGS spectra indicate that there is no spectral evidence for cooler gas with temperature below 1.0 keV in the central < 38 00 ( 52 kpc) region of A3112. High resolution RGS spectra also yields an upper limit to the turbulent motions in compact core of A3112 (185 km s 1 ). We nd that the energy contribution of turbulence to total energy is less than 5 per cent. This upper limit is consistent with the amount of energy contribution measured in recent high resolution simulations of relaxed galaxy clusters. Subject headings: X-rays: galaxies: clusters-galaxies: individual (Abell 3112)