Observations of Metals in the Intra-Cluster Medium

Werner, Norbert; Durret, F.; Ohashi, T.; Schindler, S.; Wiersma, Robert P. C.

doi:10.1007/s11214-008-9320-9

Cited by 92 publications

(76 citation statements)

References 103 publications

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“…The relative number of SN II seems to be higher in the metallicity peak region (4), and lower for the regions 2 and 3. The lowest value is obtained in the center (region 2) and it is consistent with the idea of an excess of SN Ia in the cD galaxies (Werner et al 2008). …”

Section: Sn Enrichmentsupporting

confidence: 88%

Metallicity map of the galaxy cluster A3667

Lovisari¹,

Kapferer²,

Schindler³

et al. 2009

A&A

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We use XMM-Newtondata of the merging cluster Abell 3667 to analyze its metallicity distribution. A detailed abundance map of the central 1.1 × 1.1 Mpc region indicates that metals are inhomogeneously distributed in the cluster showing a non-uniform and very complex metal pattern. The highest peak in the map corresponds to a cold region, slightly offset South of the X-ray center. This could be interpreted as stripped gas due to a merger between a group moving from NW towards the SE and the main cluster. We note several clumps of high metallicity also in the opposite direction with respect to the X-ray peak. Furthermore we determined abundances for 5 elements (O, Si, S, Ar, Fe) in four different regions of the cluster. Comparisons between these observed abundances and theoretical supernovae yields allow to get constraints on the relative number of SN Ia and II contributing to the enrichment of the intra-cluster medium. To reproduce the observed abundances of the best determined elements (Fe, O and Si) in a region of 7 around the X-ray center, 65-80% of SN II are needed. The comparison between the metal map, a galaxy density map obtained using 550 spectroscopically confirmed cluster members and, our simulations suggest a recent merger between the main cluster and the group in the SE.

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Section: Sn Enrichmentsupporting

confidence: 88%

Metallicity map of the galaxy cluster A3667

Lovisari¹,

Kapferer²,

Schindler³

et al. 2009

A&A

Self Cite

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“…Werner et al 2008, for a up-to-date review). The distribution of metals in galaxy clusters is characterized by profiles that are peaked toward the core of cooling flow clusters and rather flat in all the others (Vikhlinin et al 2005;Pratt et al 2007).…”

Section: Application To the Metal Mixing In The Icmmentioning

confidence: 99%

The mixing and transport properties of the intra cluster medium: a numerical study using tracers particles

Vazza¹,

Gheller²,

Brunetti³

2010

A&A

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We present a study of the mixing properties of the simulated intra cluster medium, using tracers particles that are advected by the gas flow during the evolution of cosmic structures. Using a sample of seven galaxy clusters (with masses in the range of M ∼ 2−3 × 10 14 M /h) simulated with a peak resolution of 25 kpc/h up to the distance of two virial radii from their centers, we investigate the application of tracers to some important problems concerning the mixing of the ICM. The transport properties of the evolving ICM are studied through the analysis of pair dispersion statistics and mixing distributions. As an application, we focus on the transport of metals in the ICM. We adopt simple scenarios for the injection of metal tracers in the ICM, and find remarkable differences of metallicity profiles in relaxed and merger systems also through the analysis of simulated emission from Doppler-shifted Fe XXIII lines.

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“…the distribution of metals in the ICM is a direct consequence of the past history of star formation in the cluster galaxies and of the processes responsible for injecting enriched gas into the ICM. (For recent reviews of the observational and theoretical aspects, see Werner et al 2008;Borgani et al 2008;Schindler & Diaferio 2008, and references therein. ) Most of the appeal of the X-rays determining elemental abundances in the hot gas stems from the apparent robustness of the measurement: most of the observed emission lines arise from well understood hydrogen-and helium-like ions and their equivalent widths can be, under the reasonable assumption of A&A 522, A34 (2010) collisional equilibrium, directly converted into the elemental abundance of the corresponding element.…”

Section: Introductionmentioning

confidence: 99%

Apparent high metallicity in 3–4 keV galaxy clusters: the inverse iron-bias in action in the case of the merging cluster Abell 2028

Gastaldello¹,

Ettori²,

Balestra³

et al. 2010

A&A

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Context. Recent work based on a global measurement of the ICM properties finds evidence for an increase in the iron abundance in galaxy clusters with temperatures around 2−4 keV up to a value about 3 times higher than is typical of very hot clusters Z Fe 0.25 Z . Aims. We have started a study of the metal distribution in nearby X-ray luminous poor galaxy clusters in the temperature range 3−4 keV with measured high abundances. Our study aims at spatially resolving the metal content of the central regions of the ICM, in particular characterizing how our measurements are biased by the diagnostics adopted and by the possible multi-temperature nature of the projected observed spectra. We report here on a 42 ks XMM-Newton observation of the first object in the sample, the cluster Abell 2028. Methods. We selected interesting regions of the ICM to analyze the spatially resolved structure of projected temperature and abundance, thereby producing two-dimensional maps. Results. The XMM-Newton observation of the first object of the sample, the cluster Abell 2028, reveals the complex structure of the cluster over a scale of ∼300 kpc, showing an interaction between two subclusters in cometary-like configurations. Cold fronts have been detected at the leading edges of the two substructures. The core of the main subcluster is likely hosting a cool corona. We show that a one-component fit for this region returns a biased high metallicity. The inverse iron bias is caused by the behavior of the fitting code in shaping the Fe-L complex. In the presence of a multi-temperature structure of the ICM, the best-fit metallicity turns out to be artificially higher when the projected spectrum is modeled with a single temperature component, while it is not related to the presence of both Fe-L and Fe-K emission lines in the spectrum. After accounting for the inverse iron bias, the overall abundance of the cluster is consistent with the one typical of hotter, more massive clusters. Conclusions. We caution against interpreting high abundances inferred when fitting a single thermal component to spectra derived from relatively large apertures in 3−4 keV clusters, because the inverse iron bias can be present. Most of the inferences trying to relate high abundances in 3−4 keV clusters to fundamental physical processes will probably have to be revised.

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Observations of Metals in the Intra-Cluster Medium

Cited by 92 publications

References 103 publications

Metallicity map of the galaxy cluster A3667

Metallicity map of the galaxy cluster A3667

The mixing and transport properties of the intra cluster medium: a numerical study using tracers particles

Apparent high metallicity in 3–4 keV galaxy clusters: the inverse iron-bias in action in the case of the merging cluster Abell 2028

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