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)
· arXiv e-print (arXiv:0708.3264)
· References in the article
· Citations to the Article (7) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (6)
· NED Objects (2)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Fields and filaments in the core of the Centaurus cluster
Authors:
Taylor, G. B.; Fabian, A. C.; Gentile, G.; Allen, S. W.; Crawford, C.; Sanders, J. S.
Affiliation:
AA(Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131, USA), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AC(Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131, USA), AD(Kavli Institute of Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA), AE(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AF(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 382, Issue 1, pp. 67-72. (MNRAS Homepage)
Publication Date:
11/2007
Origin:
MNRAS
MNRAS Keywords:
galaxies: active, galaxies: magnetic fields, galaxies: nuclei, galaxies individual: PKS1246-410, radio continuum: galaxies, X-rays: galaxies: clusters
DOI:
10.1111/j.1365-2966.2007.12368.x
Bibliographic Code:
2007MNRAS.382...67T

Abstract

We present high-resolution images of the Faraday rotation measure (RM) structure of the radio galaxy PKS1246-410at the centre of the Centaurus cluster. Comparison with Hα-line and soft X-ray emission reveals a correspondence between the line-emitting gas, the soft X-ray emitting gas, regions with an excess in the RM images and signs of depolarization. Magnetic field strengths of 25 μG, organized on scales of ~1 kpc and intermixed with gas at a temperature of 5 × 106K with a density of ~0.1 cm-3, can reproduce the observed RM excess, the depolarization and the observed X-ray surface brightness. This hot gas may be in pressure equilibrium with the optical line-emitting gas, but the magnetic field strength of 25 μG associated with the hot gas provides only 10 per cent of the thermal pressure and is therefore insufficient to account for the stability of the line-emitting filaments.
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