  We present an initial analysis of a new XMM observation of NGC 1399, the
central elliptical galaxy of the Fornax group. Spectral fitting of the
spatially resolved spectral data of the EPIC MOS and pn CCDs reveals that a
two-temperature model (2T) of the hot gas is favored over single-phase and
cooling flow models within the central ~20 kpc. The preference for the 2T model
applies whether or not the data are deprojected. The cooler component has a
temperature (~0.9 keV) similar to the kinetic temperature of the stars while
the hotter component has a temperature (~1.5 keV) characteristic of the virial
temperature of a ~10^{13} M_sun halo. The two-phase model (and other
multitemperature models) removes the ``Fe Bias'' within r < ~20 kpc and gives
Z_Fe/Z_sun 1.5-2. At larger radii the iron abundance decreases until Z_Fe/Z_sun
\~0.5 for r ~50 kpc. The Si abundance is super-solar (1.2-1.7 solar) within the
central regions while Z_Si/Z_Fe ~0.8 over the entire region studied. These Fe
and Si abundances imply that ~80% of the Fe mass within r ~50 kpc originates
from Type Ia supernovae (SNIa). This SNIa fraction is similar to that inferred
for the Sun and therefore suggests a stellar initial mass function similar to
the Milky Way.

Astrophysics