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Article overview
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On the X-ray emission of z~2 radio galaxies: IC scattering of the CMB & no evidence for fully-formed potential wells | R. A. Overzier
; D. E. Harris
; C. L. Carilli
; L. Pentericci
; H. J. A. Rottgering
; G. K. Miley
; | Date: |
1 Dec 2004 | Journal: | Astron.Astrophys. 433 (2005) 87-100 | Subject: | astro-ph | Abstract: | We present the results of 20 ksec Chandra observations for each of 5 radio galaxies in the redshift range 2.0 < z < 2.6. For 4 of the 5 targets we detect unresolved X-ray components coincident with the radio nuclei. From spectral analysis of one of the cores and comparison to the empirical radio to X-ray luminosity ratio correlation, we find that obscuring material (n(HI)~10^22 cm^-2) may be surrounding the nuclei. We detect X-ray emission coincident with the radio hotspots or lobes in 4 of the 5 targets, which can be explained by Inverse-Compton (IC) scattering of CMB photons. The magnetic field strengths of ~100-200 muG that we derive agree with the equipartition magnetic field strengths. The relative ease with which the lobe X-ray emission is detected is a consequence of the (1+z)^4 increase in the energy density of the CMB. An HST image of one of the sources shows that the X-ray emission could also be produced by a reservoir of hot, shocked gas, as evidenced by a bright, optical bow-shock. By stacking our data we created a deep, 100 ksec exposure to search for diffuse X-ray emission from intra-cluster gas. We detect no diffuse emission and derive upper limits of ~1e+44 erg/s, thereby ruling out a virialized structure of cluster-size scale at z~2. The average number of soft X-ray sources in our fields is consistent with the number density of AGN in the Chandra Deep Fields. Their angular distribution shows no evidence for large-scale structure associated with the radio galaxies. | Source: | arXiv, astro-ph/0412026 | Services: | Forum | Review | PDF | Favorites |
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