Journal Article

Abundance profiles and cool cores in galaxy groups

Ria Johnson, Alexis Finoguenov, Trevor J. Ponman, Jesper Rasmussen and Alastair J. R. Sanderson

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 413, issue 4, pages 2467-2480
Published in print June 2011 | ISSN: 0035-8711
Published online May 2011 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2011.18317.x
Abundance profiles and cool cores in galaxy groups

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Using data from the two-dimensional XMM–Newton Group Survey (2dXGS), we have examined the abundance profile properties of both cool core (CC) and non-cool core (NCC) galaxy groups. The 10 NCC systems in our sample represent a population which to date has been poorly studied in the group regime. Fitting the abundance profiles as a linear function of log radius, we find steep abundance gradients in CC systems, with a slope of −0.54 ± 0.07. In contrast, NCC groups have profiles consistent with uniform metallicity. Many CC groups show a central abundance dip or plateau, and we find evidence for anticorrelation between the core abundance gradient and the 1.4-GHz radio power of the brightest group galaxy (BGG) in CC systems. This may indicate the effect of active galactic nuclei (AGN)-driven mixing within the central ∼0.1r500. It is not possible to discern whether such behaviour is present in the NCC groups, due to the small and diverse sample with the requisite radio data. The lack of strong abundance gradients in NCC groups, coupled with their lack of CC, and evidence for enhanced substructure lead us to favour merging as the mechanism for disrupting CCs, although we cannot rule out disruption by a major AGN outburst. Given the implied time-scales, the disruptive event must have occurred within the past few Gyr in most NCC groups.

Keywords: galaxies: clusters: intracluster medium; galaxies: groups: general; X-rays: galaxies: clusters

Journal Article.  10901 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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