Chandra X-ray observations of the 3C 295 cluster core

We examine the properties of the X-ray gas in the central regions of the di stant (z = 0.46), X-ray luminous cluster of galaxies surrounding the powerf ul radio source 3C 295, using observations made with the Chandra Observator y. Between radii of 50 and 500 kpc, the cluster gas is approximately isothe rmal with an emission-weighted temperature, kT similar to5 keV. Within the central 50-kpc radius this value drops to kT similar to3.7 keV. The spectra l and imaging Chandra data indicate the presence of a cooling flow within t he central 50-kpc radius of the cluster, with a mass deposition rate of app roximately 280 M. yr(-1). We estimate an age for the cooling flow of 1-2 Gy r, which is approximately 1000 times older than the central radio source. W e find no evidence in the X-ray spectra or images for significant heating o f the X-ray gas by the radio source. We report the detection of an edge-lik e absorption feature in the spectrum for the central 50-kpc region, which m ay be caused by oxygen-enriched dust grains. The implied mass in metals see n in absorption could have been accumulated by the cooling flow over its li fetime. Combining the results on the X-ray gas density profile with radio m easurements of the Faraday rotation measure in 3C 295, we estimate the magn etic field strength in the region of the cluster core to be B similar to 12 muG.