High Resolution XMM-Newton Spectroscopy of the Cooling Flow Cluster
  A3112
  We examine high signal to noise XMM-Newton European Photon Imaging Camera
(EPIC) and Reflection Grating Spectrometer (RGS) observations to determine the
physical characteristics of the gas in the cool core and outskirts of the
nearby rich cluster A3112. The XMM-Newton Extended Source Analysis Software
data reduction and background modeling methods were used to analyze the XMM-
Newton EPIC data. From the EPIC data we find that the iron and silicon
abundance gradients show significant increase towards the center of the cluster
while the oxygen abundance profile 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 f_gas= 0.149^{+0.036}_{-0.032} at R500,
is consistent with the seven-year WMAP results. The comparisons of line fluxes
and flux 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
associated with the cluster with temperature below 1.0 keV in the central <38"
(\sim 52 kpc) region of A3112. High resolution RGS spectra also yield an upper
limit to the turbulent motions in compact core of A3112 (206 km/s). We find
that the energy contribution of turbulence to total energy is less than 6 per
cent. This upper limit is consistent with the amount of energy contribution
measured in recent high resolution simulations of relaxed galaxy clusters.
