We present an analysis of Chandra observations of the central regions of the cooling flow cluster Abell 2029 .
We find a number of X-ray filaments in the central 40 kpc , some of which appear to be associated with the currently active central radio galaxy .
The outer southern lobe of the steep-spectrum radio source appears to be surrounded by a region of cool gas and is at least partially surrounded by a bright X-ray rim similar to that seen around radio sources in the cores of other cooling flow clusters .
Spectroscopic fits show that the overall cluster emission is best fitted by either a two temperature gas ( kT _ { high } = 7.47 keV , kT _ { low } = 0.11 keV ) , or a cooling flow model with gas cooling over the same temperature range .
This large range of temperatures ( over a factor of 50 ) is relatively unique to Abell 2029 and may suggest that this system is a very young cooling flow where the gas has only recently started cooling to low temperatures .
The cooling flow model gives a mass deposition rate of \dot { M } = 56 ^ { +16 } _ { -21 } \mbox { $M _ { \odot } $ } yr ^ { -1 } .
In general , the cluster emission is elongated along a position angle of 22° with an ellipticity of 0.26 .
The distribution of the X-ray emission in the central region of the cluster is asymmetric , however , with excess emission to the north-east and south-east compared to the south-west and north-west , respectively .
Fitting and subtracting a smooth elliptical model from the X-ray data reveals a dipolar spiral excess extending in a clockwise direction from the cluster core to radii of \sim 150 kpc .
We estimate a total mass of M _ { spiral } \sim 6 \times 10 ^ { 12 } M _ { \odot } in the spiral excess .
The most likely origins of the excess are either stripping of gas from a galaxy group or bare dark matter potential which has fallen into the cluster , or sloshing motions in the cluster core induced by a past merger .