We present the results of a Chandra observation of the central region of Abell 3112 .
This cluster has a powerful radio source in the center and was believed to have a strong cooling flow .
The X-ray image shows that the intracluster medium ( ICM ) is distributed smoothly on large scales , but has significant deviations from a simple concentric elliptical isophotal model near the center .
Regions of excess emission appear to surround two lobe-like radio-emitting regions .
This structure probably indicates that hot X-ray gas and radio lobes are interacting .
From an analysis of the X-ray spectra in annuli , we found clear evidence for a temperature decrease and abundance increase toward the center .
The X-ray spectrum of the central region is consistent with a single-temperature thermal plasma model .
The contribution of X-ray emission from a multiphase cooling flow component with gas cooling to very low temperatures locally is limited to less than 10 % of the total emission .
However , the whole cluster spectrum indicates that the ICM is cooling significantly as a whole , but in only a limited temperature range ( \geq 2 keV ) .
Inside the cooling radius , the conduction timescales based on the Spitzer conductivity are shorter than the cooling timescales .
We detect an X-ray point source in the cluster center which is coincident with the optical nucleus of the central cD galaxy and the core of the associated radio source .
The X-ray spectrum of the central point source can be fit by a 1.3 keV thermal plasma and a power-law component whose photon index is 1.9 .
The thermal component is probably plasma associated with the cD galaxy .
We attribute the power-law component to the central AGN .