The metallicity of the intracluster medium over cosmic time: further evidence for early enrichment

Mantz, Adam; Allen, S. W.; Morris, R. Glenn; Simionescu, A.; Urban, O.; Werner, Norbert; Zhuravleva, Irina

doi:10.1093/mnras/stx2200

Cited by 64 publications

(99 citation statements)

References 47 publications

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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%

“…average kT 3 keV), so it is not representative of the whole cluster population. Other recent studies (Ettori et al 2015, McDonald et al 2016, Mantz et al 2017, although more focused on the evolution of the metallicity with redshift, found a trend of higher metallicity in the innermost regions of cool-core clusters with respect to noncool-core systems. Moreover, the metallicity in the core was found to be much higher than the metallicity in the outskirts for both relaxed and disturbed systems (e.g.…”

Section: Introductionmentioning

confidence: 87%

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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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Section: Introductionsupporting

confidence: 68%

Section: Introductionmentioning

confidence: 87%

The non-uniformity of galaxy cluster metallicity profiles

Lovisari

Reiprich

2018

Monthly Notices of the Royal Astronomical Society

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“…NCC clusters, however, have a flat distribution in the core and follow the same universal distribution as CC for outer radii. 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.…”

Section: Introductionmentioning

confidence: 80%

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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“…More difficult to reconcile are the results by Mantz et al (2017), where no evolution is found in the very [0-0.1] and in the [0.5-1] r 500 radial range, while a mild but very significant evolution is found for the range [0.1-0.5] r 500 . If we try to average their [0.1-0.5] r 500 and [0.5-1] r 500 bins, however, we find γ = 0.51 ± 0.46 which is again consistent with our findings.…”

Section: Comparison With Previous Workmentioning

confidence: 90%

The chemical evolution of galaxy clusters: Dissecting the iron mass budget of the intracluster medium

Liu

Tozzi

Ettori

et al. 2020

A&A

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Aims. We study the chemical evolution of galaxy clusters by measuring the iron mass in the ICM after dissecting the abundance profiles into different components. Methods. We use Chandra archival observations of 186 morphologically regular clusters in the redshift range [0.04, 1.07]. For each cluster we compute the azimuthally-averaged iron abundance and gas density profiles. In particular, we aim at identifying a central peak in the iron distribution, associated with the central galaxy, and an approximately constant plateau reaching the largest observed radii, possibly associated with early enrichment occurred before and/or shortly after the virialization of the cluster. We are able to firmly identify the two components in the iron distribution in a significant fraction of the sample, simply relying on the fit of the iron abundance profile. From the abundance and ICM density profiles we compute the iron mass included in the iron peak and iron plateau, and the gas mass-weighted iron abundance of the ICM, out to an extraction radius of 0.4 r 500 and, extending the abundance profile as a constant, to r 500 . Results. We find that the iron plateau shows no evolution with redshift. On the other hand, we find marginal (< 2σ c.l.) decrease with redshift in the iron mass included in the iron peak rescaled by the gas mass. We measure that the fraction of iron peak mass is typically a few percent (∼ 1%) of the total iron mass within r 500 . Therefore, since the total iron mass budget is dominated by the plateau, we find consistently that the global gas mass-weighted iron abundance does not evolve significantly across our sample. We are also able to reproduce past claims of evolution in the global iron abundance, which turn out to be due to the use of cluster samples with different selection methods combined to the use of emission-weighted instead of gas mass-weighted abundance values. Finally, while the intrinsic scatter in the iron plateau mass is consistent with zero, the iron peak mass exhibits a large scatter, in line with the fact that the peak is produced after the virialization of the halo and depends on the formation history of the hosting cool core and the strength of the associated feedback processes. Conclusions. We conclude that only a spatially-resolved approach can resolve the issue of the iron abundance evolution in the ICM, reconciling the contradictory results obtained in the last ten years. Evolutionary effects below z ∼ 1 are marginally measurable with present-day data, while at z > 1 the constraints are severely limited by the poor knowledge of the high-z cluster population. The path towards a full and comprehensive chemical history of the ICM necessarily requires the use of high-angular resolution X-ray bolometers and a dramatic increase in the statistics of faint, extended X-ray sources.

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The metallicity of the intracluster medium over cosmic time: further evidence for early enrichment

Cited by 64 publications

References 47 publications

The non-uniformity of galaxy cluster metallicity profiles

The non-uniformity of galaxy cluster metallicity profiles

Iron abundance distribution in the hot gas of merging galaxy clusters

The chemical evolution of galaxy clusters: Dissecting the iron mass budget of the intracluster medium

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