  We use a deep XMM-Newton Reflection Grating Spectrometer observation to
examine the X-ray emission from the core of the Centaurus cluster of galaxies.
We clearly detect Fe-XVII emission at four separate wavelengths, indicating the
presence of cool X-ray emitting gas in the core of the cluster. Fe ions from
Fe-XVII to XXIV are observed. The ratio of the Fe-XVII 17.1A lines to 15.0A
line and limits on O-VII emission indicate a lowest detected temperature in the
emitting region of 0.3 to 0.45 keV (3.5 to 5.2x10^6 K). The cluster also
exhibits strong N-VII emission, making it apparent that the N abundance is
supersolar in its very central regions. Comparison of the strength of the
Fe-XVII lines with a Solar metallicity cooling flow model in the inner 17 kpc
radius gives mass deposition rates in the absence of heating of 1.6-3 Msun/yr.
Spectral fitting implies an upper limit of 0.8 Msun/yr below 0.4 keV, 4 Msun/yr
below 0.8 keV and 8 Msun/yr below 1.6 keV. The cluster contains X-ray emitting
gas over at least the range of 0.35 to 3.7 keV, a factor of more than 10 in
temperature. We find that the best fitting metallicity of the cooler components
is smaller than the hotter ones, confirming that the apparent metallicity does
decline within the inner 1 arcmin radius.
