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Chandra X-ray observations of the 3C295 cluster core | | S.W. Allen
; G.B. Taylor
; P.E.J. Nulsen
; R.M. Johnstone
; L.P. David
; S. Ettori
; A.C. Fabian
; W. Forman
; C. Jones
; B. McNamara
; | | Date: |
10 Dec 2000 | | Journal: | Mon.Not.Roy.Astron.Soc. 324 (2001) 842 | | Subject: | astro-ph | | Abstract: | We examine the properties of the X-ray gas in the central regions of the distant (z=0.46), X-ray luminous cluster of galaxies surrounding the powerful radio source 3C 295, using observations made with the Chandra Observatory. Between radii of 50-500 kpc, the cluster gas is approximately isothermal with an emission-weighted temperature, kT ~5 keV. Within the central 50 kpc radius this value drops to kT ~3.7 keV. The spectral and imaging Chandra data indicate the presence of a cooling flow within the central 50 kpc radius of the cluster, with a mass deposition rate of approximately 280 solar masses per year. We estimate an age for the cooling flow of 1-2 Gyr, which is approximately one thousand times older than the central radio source. We find no evidence in the X-ray spectra or images for significant heating of the X-ray gas by the radio source. We report the detection of an edge-like absorption feature in the spectrum for the central 50 kpc region, which may be due to oxygen-enriched dust grains. The implied mass in metals seen in absorption could have been accumulated by the cooling flow over its lifetime. Combining the results on the X-ray gas density profile with radio measurements of the Faraday rotation measure in 3C295, we estimate the magnetic field strength in the region of the cluster core to be B ~12 muG. | | Source: | arXiv, astro-ph/0101162 | | Services: | Forum | Review | PDF | Favorites | |
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