Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· arXiv e-print (arXiv:astro-ph/0301468)
· On-line Data
· References in the article
· Citations to the Article (43) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (7)
· NED Objects (2)
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
A deep Chandra observation of the cluster environment of the z= 1.786 radio galaxy 3C 294
Authors:
Fabian, A. C.; Sanders, J. S.; Crawford, C. S.; Ettori, S.
Affiliation:
AA(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AC(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AD(ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching b. Munchen, Germany)
Publication:
Monthly Notice of the Royal Astronomical Society, Volume 341, Issue 3, pp. 729-738. (MNRAS Homepage)
Publication Date:
05/2003
Origin:
MNRAS
MNRAS Keywords:
galaxies: active, galaxies: clusters: individual: 3C 294, intergalactic medium, X-rays: galaxies
DOI:
10.1046/j.1365-8711.2003.06394.x
Bibliographic Code:
2003MNRAS.341..729F

Abstract

We report the results from a 200-ks Chandra observation of the z= 1.786 radio galaxy 3C 294 and its cluster environment, increasing by ten-fold our earlier observation. The diffuse emission, extending about 100 kpc around the nucleus, has a roughly hourglass shape in the north-south (N-S) direction with surprisingly sharp edges to the N and S. The spectrum of the diffuse emission is well fitted by either a thermal model of temperature 3.5 keV and abundance <0.9 Zsolar (2σ), or a power law with photon index 2.3. If the emission is due to hot gas then the sharp edges mean that it is probably not in hydrostatic equilibrium. Much of the emission is plausibly due to inverse Compton scattering of the cosmic microwave background (CMB) by non-thermal electrons produced earlier by the radio source. The required relativistic electrons would be of much lower energy and older than those responsible for the present radio lobes. This could account for the lack of detailed spatial correspondence between the X-rays and the radio emission, the axis of which is at a position angle of about 45°. Hot gas would still be required to confine the relativistic plasma; the situation could parallel that of the radio bubbles seen as holes in nearby clusters, except that in 3C 294 the bubbles are bright in X-rays owing to the extreme power in the source and the sixty-fold increase in the energy density of the CMB. The X-ray spectrum of the radio nucleus is hard, showing a reflection spectrum and iron line. The source is therefore an obscured radio-loud quasar.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints