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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  17.1 Å lines to 15.0 Å 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  5.2 × 10 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 M ⊙  yr −1  . Spectral fitting implies an upper limit of  0.8  M ⊙  yr −1   below 0.4 keV,  4   M ⊙  yr −1   below 0.8 keV and  8  M ⊙   yr −1   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.

Cool X‐ray emitting gas in the core of the Centaurus cluster of galaxies