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Reference: Sanders, JS, Fabian, AC, Taylor, GB et al., (2016). A very deep Chandra view of metals, sloshing and feedback in the Centaurus cluster of galaxies. Monthly Notices of the Royal Astronomical Society, 457 (1), 82-109.Citable link to this page:


A very deep Chandra view of metals, sloshing and feedback in the Centaurus cluster of galaxies

Abstract: We examine deep Chandra X-ray observations of the Centaurus cluster ofgalaxies, Abell 3526. Applying a gradient magnitude filter reveals a wealth ofstructure, from filamentary soft emission on 100pc (0.5 arcsec) scales close tothe nucleus to features 10s of kpc in size at larger radii. The clustercontains multiple high-metallicity regions with sharp edges. Relative to anazimuthal average, the deviations of metallicity and surface brightness arecorrelated, and the temperature is inversely correlated, as expected if thelarger scale asymmetries in the cluster are dominated by sloshing motions.Around the western cold front are a series of ~7 kpc 'notches', suggestive ofKelvin-Helmholtz instabilities. The cold front width varies from 4 kpc down toclose to the electron mean free path. Inside the front are multiple metallicityblobs on scales of 5-10 kpc, which could have been uplifted by AGN activity,also explaining the central metallicity drop and flat inner metallicityprofile. Close to the nucleus are multiple shocks, including a 1.9-kpc-radiusinner shell-like structure and a weak 1.1-1.4 Mach number shock around thecentral cavities. Within a 10 kpc radius are 9 depressions in surfacebrightness, several of which appear to be associated with radio emission. Theshocks and cavities imply that the nucleus has been repeatedly active on 5-10Myr timescales, indicating a tight balance between heating and cooling. Weconfirm the presence of a series of linear quasi-periodic structures. If theyare sound waves, the ~5 kpc spacing implies a period of 6 Myr, similar to theages of the shocks and cavities. Alternatively, these structures may beKelvin-Helmholtz instabilities, their associated turbulence or amplifiedmagnetic field layers.

Peer Review status:Peer reviewedPublication status:PublishedVersion:Publisher's version Funder: NASA   Notes:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Bibliographic Details

Publisher: Oxford University Press

Publisher Website: http://www.oxfordjournals.org/


Publisher Website: http://dx.doi.org/10.1093/mnras/stv2972

Journal: Monthly Notices of the Royal Astronomical Societysee more from them

Publication Website: http://mnras.oxfordjournals.org/

Issue Date: 2016


Urn: uuid:f824db60-c5f0-4d78-941f-56a5a47fe9bc

Source identifier: 589567

Eissn: 1365-2966

Doi: https://doi.org/10.1093/mnras/stv2972

Issn: 0035-8711 Item Description

Type: Journal article;

Version: Publisher's versionKeywords: galaxies: clusters: individual: Abell 3526 X-rays: galaxies: clusters astro-ph.HE Tiny URL: pubs:589567


Author: Sanders, JS - - - Fabian, AC - - - Taylor, GB - - - Russell, HR - - - Blundell, KM - institutionUniversity of Oxford Oxford, MPLS

Source: https://ora.ox.ac.uk/objects/uuid:f824db60-c5f0-4d78-941f-56a5a47fe9bc


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