Uniform Contribution of Supernova Explosions to the Chemical Enrichment of Abell 3112 out to R<sub>200</sub>

Ezer, Cemile; Bulbul, Esra; Ercan, E. N.; Bautz, M. W.; Loewenstein, M.; McDonald, M.; Miller, Eric D.

doi:10.3847/1538-4357/836/1/110

Cited by 30 publications

(30 citation statements)

References 53 publications

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“…14). Combined with the previous observations of a uniform ∼0.3 Z Fe abundance in the outskirts of (mostly) CC clusters (Fujita et al 2008;Werner et al 2013;Thölken et al 2016;Urban et al 2017;Ezer et al 2017), we conclude that Fe distribution in cluster outskirts of these merging clusters depends very weakly (or not at all) on the dynamical state of the cluster. This has important consequences regarding the chemical history of large-scale structures.…”

Section: Abundance Vs Pseudo-entropy Relationsupporting

confidence: 88%

“…These abundance distributions do not present evidence of evolution up to z ∼ 1 (McDonald et al 2016;Mantz et al 2017;Ettori et al 2017). Moreover, recent X-ray observations with Suzaku (Fujita et al 2008;Werner et al 2013;Urban et al 2017;Ezer et al 2017;Simionescu et al 2017) reveal an uniform radial distribution around ∼0.2-0.3 Z in the outskirts of the galaxy clusters, which suggests an early enrichment of the ICM (i.e. z ∼ 2-3).…”

Section: Introductionmentioning

confidence: 79%

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Iron abundance distribution in the hot gas of merging galaxy clusters

Urdampilleta

Mernier

Kaastra

et al. 2019

A&A

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We present XMM-Newton/EPIC observations of six merging galaxy clusters and study the distributions of their temperature, iron (Fe) abundance and pseudo-entropy along the merging axis. For the first time, we focus simultaneously, and in a comprehensive way, on the chemical and thermodynamic properties of the freshly collided intracluster medium (ICM). The Fe distribution of these clusters along the merging axis is found to be in good agreement with the azimuthally-averaged Fe abundance profile in typical non-cool-core clusters out to r 500 . In addition to showing a moderate central abundance peak, though less pronounced than in relaxed systems, the Fe abundance flattens at large radii towards ∼0.2-0.3 Z . Although this shallow metal distribution is in line with the idea that disturbed, non-cool-core clusters originate from the merging of relaxed, cool-core clusters, we find that in some cases, remnants of metal-rich and low entropy cool cores can persist after major mergers. While we obtain a mild anti-correlation between the Fe abundance and the pseudo-entropy in the (lower entropy, K = 200-500 keV cm 2 ) inner regions, no clear correlation is found at (higher entropy, K = 500-2300 keV cm 2 ) outer radii. The apparent spatial abundance uniformity that we find at large radii is difficult to explain through an efficient mixing of freshly injected metals, particularly in systems for which the time since the merger is short. Instead, our results provide important additional evidence in favour of the early enrichment scenario -in which the bulk of the metals are released outside galaxies at z > 2-3 -and extend it from cool-core and (moderate) non-cool-core clusters to a few of the most disturbed merging clusters as well. These results constitute a first step towards a deeper understanding of the chemical history of merging clusters.

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Section: Abundance Vs Pseudo-entropy Relationsupporting

confidence: 88%

Section: Introductionmentioning

confidence: 79%

Iron abundance distribution in the hot gas of merging galaxy clusters

Urdampilleta

Mernier

Kaastra

et al. 2019

A&A

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“…Suzaku XIS observations of the Perseus cluster in 78 independent spatial bins and along 8 azimuthal directions revealed a uniform iron abundance of Z Fe = 0.304 ± 0.012 proto-solar, as a function of both azimuth and radius, out to r 200 (Werner et al 2013). Very deep Suzaku observations of Abell 3112 (Ezer et al 2017) as well as the analysis of archival Suzaku data for the outskirts of ten massive clusters ) confirm the results of the Perseus observations. find that, across their sample, the Fe abundances are consistent with a constant value, Z Fe = 0.306 ± 0.012 proto-solar, which is remarkably similar to the value measured for the Perseus cluster.…”

Section: Metals In Cluster Outskirtssupporting

confidence: 73%

“…From the same respective studies, the red circles and the red shaded area show the intrinsic scatter of the measurements (following the method of ). The black dotted line, the yellow triangles, the green squares, and the black stars show respectively the Suzaku XIS measurements of the outskirts of the Perseus cluster (Werner et al 2013, averaged value), the UGC 03957 group (Thölken et al 2016), the A 3112 cluster (Ezer et al 2017), and the Virgo cluster , azimuthally averaged along the N, S, and W arms). All the abundances are rescaled with respect to the proto-solar values of Lodders et al (2009). Rgs Sample (CHEERS), including clusters, groups, and massive ellipiticals -and showed that their azimuthally averaged SNIa-to-SNcc contribution remains remarkably uniform out to at least ∼0.5 r 500 .…”

Section: Central Abundance Distributionmentioning

confidence: 99%

Enrichment of the Hot Intracluster Medium: Observations

et al. 2018

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Four decades ago, the firm detection of an Fe-K emission feature in the X-ray spectrum of the Perseus cluster revealed the presence of iron in its hot intracluster medium (ICM). With more advanced missions successfully launched over the last 20 years, this discovery has been extended to many other metals and to the hot atmospheres of many other galaxy clusters, groups, and giant elliptical galaxies, as evidence that the elemental bricks of life -synthesized by stars and supernovae -are also found at the largest scales of the Universe. Because the ICM, emitting in X-rays, is in collisional ionisation equilibrium, its elemental abundances can in principle be accurately measured. These abundance measurements, in turn, are valuable to constrain the physics and environmental conditions of the Type Ia and core-collapse supernovae that exploded and enriched the ICM over the entire cluster volume. On the other hand, the spatial distribution of metals across the ICM constitutes a remarkable signature of the chemical history and evolution of clusters, groups, and ellipticals. Here, we summarise the most significant achievements in measuring elemental abundances in the ICM, from the very first attempts up to the era of XMM-Newton, Chandra, and Suzaku and the unprecedented results obtained by Hitomi. We also discuss the current systematic limitations of these measurements and how the future missions XRISM and Athena will further improve our current knowledge of the ICM enrichment.

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“…Beyond that radius, the metallicity is consistent with being flat, as shown by the measurements of the ICM metallicity up to the virial radius for several clusters (e.g. Fujita et al 2008, Werner et al 2013, Simionescu et al 2015, Thölken et al 2016, Ezer et al 2017, Urban et al 2017.…”

Section: Introductionsupporting

confidence: 68%

The non-uniformity of galaxy cluster metallicity profiles

Lovisari

Reiprich

2018

Monthly Notices of the Royal Astronomical Society

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We study a sample of 207 nearby galaxy groups and clusters observed with XMM-Newton. Key aspects of this sample include the large size, the high data quality, and the large diversity of cluster dynamical states. We determine the overall metallicity within 0.3R 500 and the radial distribution of the metals. On average, we find a mild dependence of the core metallicity with the average temperature of the system in agreement with previous results. However, we identify the cause of this mild dependence to be due to relaxed systems only; disturbed systems do not show this trend, on average. The large scatter observed in this relation is strongly associated with the dynamical state of the systems: relaxed systems have on average a higher metallicity in the core than disturbed objects. The radial profiles of relaxed systems are centrally peaked and show a steep decrease with radius, flattening beyond 0.3-0.4R 500 . The metallicity of disturbed systems is also higher in the center but at much lower values than what is observed for relaxed objects. This finding is consistent with the picture that cluster mergers mix the abundance distribution by inducing large scale motions. The scatter of the radial profiles is quite large, but while for relaxed systems it decreases almost monotonically as function of the radius, for disturbed systems it shows a significant boost at large radii. Systems with a central radio source have a flatter profile indicating that central AGNs are an efficient mechanism to uplift and redistribute the metals in the ICM.

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Uniform Contribution of Supernova Explosions to the Chemical Enrichment of Abell 3112 out to R₂₀₀

Cited by 30 publications

References 53 publications

Iron abundance distribution in the hot gas of merging galaxy clusters

Iron abundance distribution in the hot gas of merging galaxy clusters

Enrichment of the Hot Intracluster Medium: Observations

The non-uniformity of galaxy cluster metallicity profiles

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Uniform Contribution of Supernova Explosions to the Chemical Enrichment of Abell 3112 out to R200

Cited by 30 publications

References 53 publications

Iron abundance distribution in the hot gas of merging galaxy clusters

Iron abundance distribution in the hot gas of merging galaxy clusters

Enrichment of the Hot Intracluster Medium: Observations

The non-uniformity of galaxy cluster metallicity profiles

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Product

Resources

About

Uniform Contribution of Supernova Explosions to the Chemical Enrichment of Abell 3112 out to R₂₀₀