Gas sloshing, cold fronts, Kelvin-Helmholtz instabilities and the merger history of the cluster of galaxies Abell 496

Röediger, E.; Lovisari, Lorenzo; Dupke, Renato A.; Ghizzardi, S.; Brüggen, M.; Kraft, Ralph; Macháček, M.

doi:10.1111/j.1365-2966.2011.20287.x

Cited by 89 publications

(91 citation statements)

References 39 publications

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“…Bîrzan et al 2012) and the depths (Fe(r max )/Fe drop ) or the radial extent (r max /r 500 ) of the drops in our sample. Similarly, while the extended drop seen in NGC 5044 might be partly explained by its peculiar metal distribution in the sloshed gas (O'Sullivan et al 2014), sloshing process can probably not explain the (narrower) drops seen in other objects (Roediger et al 2011(Roediger et al , 2012.…”

Section: Central Metallicity Dropmentioning

confidence: 99%

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

Mernier

Plaa

Kaastra

et al. 2017

A&A

117

161

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The hot intra-cluster medium (ICM) permeating galaxy clusters and groups is not pristine, as it has been continuously enriched by metals synthesised in Type Ia (SNIa) and core-collapse (SNcc) supernovae since the major epoch of star formation (z 2-3). The cluster/group enrichment history and mechanisms responsible for releasing and mixing the metals can be probed via the radial distribution of SNIa and SNcc products within the ICM. In this paper, we use deep XMM-Newton/EPIC observations from a sample of 44 nearby cool-core galaxy clusters, groups, and ellipticals (CHEERS) to constrain the average radial O, Mg, Si, S, Ar, Ca, Fe, and Ni abundance profiles. The radial distributions of all these elements, averaged over a large sample for the first time, represent the best constrained profiles available currently. Specific attention is devoted to a proper modelling of the EPIC spectral components, and to other systematic uncertainties that may affect our results. We find an overall decrease of the Fe abundance with radius out to ∼0.9r 500 and ∼0.6r 500 for clusters and groups, respectively, in good agreement with predictions from the most recent hydrodynamical simulations. The average radial profiles of all the other elements (X) are also centrally peaked and, when rescaled to their average central X/Fe ratios, follow well the Fe profile out to at least ∼0.5r 500 . As predicted by recent simulations, we find that the relative contribution of SNIa (SNcc) to the total ICM enrichment is consistent with being uniform at all radii, both for clusters and groups using two sets of SNIa and SNcc yield models that reproduce the X/Fe abundance pattern in the core well. In addition to implying that the central metal peak is balanced between SNIa and SNcc, our results suggest that the enriching SNIa and SNcc products must share the same origin and that the delay between the bulk of the SNIa and SNcc explosions must be shorter than the timescale necessary to diffuse out the metals. Finally, we report an apparent abundance drop in the very core of 14 systems (∼32% of the sample). Possible origins of these drops are discussed.

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Section: Central Metallicity Dropmentioning

confidence: 99%

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

Mernier

Plaa

Kaastra

et al. 2017

A&A

117

161

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“…The ICM is rarely in perfect hydrostatic equilibrium because large-scale accretion of matter, turbulent motions, gas sloshing, AGN, and galaxy motions are considerably and regularly perturbing the gas (e.g., Schuecker et al 2004, Henry et al 2004Vogt & Enßlin 2005;Enßlin & Vogt 2006;Sanders et al 2010;Roediger et al 2012). …”

Section: Metallicity In Cluster Outskirtsmentioning

confidence: 99%

Outskirts of Galaxy Clusters

et al. 2013

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Until recently, only about 10% of the total intracluster gas volume had been studied with high accuracy, leaving a vast region essentially unexplored. This is now changing and a wide area of hot gas physics and chemistry awaits discovery in galaxy cluster outskirts. Also, robust large-scale total mass profiles and maps are within reach. First observational and theoretical results in this emerging field have been achieved in recent years with sometimes surprising findings. Here, we summarize and illustrate the relevant underlying physical and chemical processes and review the recent progress in X-ray, Sunyaev-Zel'dovich, and weak gravitational lensing observations of cluster outskirts, including also brief discussions of technical challenges and possible future improvements.Keywords Galaxy clusters · large-scale structure of the Universe · intracluster matter

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“…Markevitch & Vikhlinin 2007). Roediger et al (2012a) found that the boxy structure in A496 arises due to the development of Kelvin-Helmholtz instabilities along cold fronts. The cold front appears strongest around the N edge of the SW group core where the outer hot atmospheres of each group are colliding.…”

Section: Spatially Resolved Spectroscopymentioning

confidence: 99%

The bow shock, cold fronts and disintegrating cool core in the merging galaxy group RX J0751.3+5012

Russell¹,

Fabian²,

McNamara³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Gas sloshing, cold fronts, Kelvin-Helmholtz instabilities and the merger history of the cluster of galaxies Abell 496

Cited by 89 publications

References 39 publications

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

Outskirts of Galaxy Clusters

The bow shock, cold fronts and disintegrating cool core in the merging galaxy group RX J0751.3+5012

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