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 \sim 20 kpc .
The preference for the 2T model applies whether or not the data are deprojected .
The cooler component has a temperature ( \sim 0.9 keV ) similar to the kinetic temperature of the stars while the hotter component has a temperature ( \sim 1.5 keV ) characteristic of the virial temperature of a \sim 10 ^ { 13 } \hbox { { $M _ { \sun } $ } } halo .
The two-phase model ( and other multitemperature models ) removes the “ Fe Bias ” within r \lesssim 20 kpc and gives \hbox { { $Z _ { Fe } $ } } / \hbox { { $Z _ { \odot } $ } } \approx 1.5 - 2 .
At larger radii the iron abundance decreases until \hbox { { $Z _ { Fe } $ } } / \hbox { { $Z _ { \odot } $ } } \sim 0.5 for r \sim 50 kpc .
The Si abundance is super-solar ( 1.2-1.7 solar ) within the central regions while \hbox { { $Z _ { Si } $ } } / \hbox { { $Z _ { Fe } $ } } \approx 0.8 over the entire region studied .
These Fe and Si abundances imply that \approx 80 \% of the Fe mass within r \sim 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 .