We present an analysis of the Chandra X-ray observation of Abell 2052 , including large scale properties of the cluster as well as the central region which includes the bright radio source , 3C 317 .
We present temperature and abundance profiles using both projected and deprojected spectral analyses .
The cluster shows the cooling flow signatures of excess surface brightness above a \beta -model at the cluster center , and a temperature decline into the center of the cluster .
For Abell 2052 , the temperature drops by a factor of three from approximately 3 to 1 keV .
The heavy element abundances initially increase into the center , but decline within 30″ .
Temperature and abundance maps show that the X-ray bright shells surrounding the radio source are the coolest and least abundant regions in the cluster .
The mass-deposition rate in the cooling flow is 26 < \dot { M } < 42 ~ { } M _ { \odot } yr ^ { -1 } .
This rate is approximately a factor of three lower than the rates found with previous X-ray observatories .
Based on a stellar population analysis using imaging and spectra at wavelengths spanning the far ultraviolet to the near infrared , we find a star formation rate of 0.6 ~ { } M _ { \odot } yr ^ { -1 } within a 3 \arcsec radius of the nucleus of the central cluster galaxy .
Total and gas mass profiles for the cluster are also determined .
We investigate additional sources of pressure in the X-ray holes formed by the radio source , and limit the temperature of any hot , diffuse , thermal component which provides the bulk of the pressure in the holes to kT \gtrsim 20 keV .
We calculate the magnetic field in the bright-shell region and find B \approx 11 ~ { } \mu G. The magnetic pressure in the cluster center is significantly lower than the gas pressure .
The current luminosity of the central AGN is L _ { X } = 7.9 \times 10 ^ { 41 } erg s ^ { -1 } , and its spectrum is well-fitted by a power-law model with no excess absorption above the Galactic value .
The energy output from several radio outbursts , occurring episodically over the lifetime of the cluster , may be sufficient to offset the cooling flow near the center .