We present Chandra data from a 31.7 ks observation of the Centaurus cluster , using the ACIS-S detector .
Images of the X-ray emission show a plume-like feature at the centre of the cluster , of extent 60 arcsec ( 20 kpc in projection ) .
The feature has the same metallicity as gas at a similar radius , but is cooler .
Using adaptive binning , we generate temperature , abundance and absorption maps of the cluster core .
The radial abundance profile shows that the previously known , steep abundance gradient peaks with a metallicity of 1.3 - 1.8 \hbox { $ \thinspace \mathrm { Z } _ { \odot } $ } at a radius of about 45 arcsec ( 15 kpc ) , before falling back to 0.4 \hbox { $ \thinspace \mathrm { Z } _ { \odot } $ } at the centre of the cluster .
A radial temperature profile shows that the temperature decreases inwards .
We determine the spatial distributions of each of two temperature components , where applicable .
The radiative cooling time of the cooler component within the inner 10 arcsec ( 3 kpc ) is less than 2 \times 10 ^ { 7 } yr. X-ray holes in the image coincident with the radio lobes are seen , as well as two outer sharp temperature drops , or cold fronts .
The origin of the plume is unclear .
The existence of the strong abundance gradient is a strong constraint on extensive convection or gas motion driven by a central radio source .