The Chemical Enrichment of the ICM from Hydrodynamical Simulations

Borgani, S.; Fabjan, D.; Tornatore, L.; Schindler, S.; Dolag, K.; Diaferio, Antonaldo

doi:10.1007/s11214-008-9322-7

Cited by 61 publications

(49 citation statements)

References 89 publications

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“…The major sources of Fe in the Universe are type-Ia supernovae (SNIa), whereas other elements (alpha elements) are produced by core-collapsed SN (SNcc) or by a mix of the two SN types. A measure of the alpha/Fe ratios in the ICM gives a first-order approximation of the relative importance of the SN types to the enrichment (for a review see Werner et al 2008;Borgani et al 2008). Early claims of an increasing type-Ia supernovae (SNIa) contribution, with respect to the SN core-collapsed (SNcc) to the ICM enrichment towards cluster centres (Finoguenov et al 2000;Rasmussen & Ponman 2007), contributed to establishing a scenario where the Fe abundance in cores increased steadily from the time of formation to z = 0 (e.g.…”

Section: Introductionmentioning

confidence: 99%

On the Fe abundance peak formation in cool-core clusters of galaxies: hints from cluster WARPJ1415.1+3612 atz= 1.03

Grandi

Santos

Nonino

et al. 2014

A&A

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We present a detailed study of the iron content of the core of the high-redshift cluster WARPJ1415.1+3612 (z = 1.03). By comparing the central Fe mass excess observed in this system, M exc Fe = (1.67 ± 0.40) × 10 9 M , with those measured in local cool-core systems, we infer that the bulk of the mass excess was already in place at z = 1, when the age of the Universe was about half of what it is today. Our measures point to an early and intense period of star formation most likely associated with the formation of the BCG. Indeed, in the case of the power-law delay time distribution with slope −1, which reproduces the data of WARPJ1415.1+3612 best, half of the supernovae explode within 0.4 Gyr of the formation of the BCG. Finally, while for local cool-core clusters the Fe distribution is broader than the near-infrared light distribution of the BCG, in WARPJ1415.1+3612 the two distributions are consistent, indicating that the process responsible for broadening the Fe distribution in local systems has not yet started in this distant cluster.

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Section: Introductionmentioning

confidence: 99%

On the Fe abundance peak formation in cool-core clusters of galaxies: hints from cluster WARPJ1415.1+3612 atz= 1.03

Grandi

Santos

Nonino

et al. 2014

A&A

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“…the physical condition of the ICM at the epoch of the enrichment) and cannot be obtained directly from X-ray observations, the radial distribution of metals in the ICM, as well as their abundance as a function of time, represent the "footprint" of cosmic star formation history and are crucial to trace the effect of SN feedback on the ICM at different cosmic epochs (e.g. Ettori 2005;Borgani et al 2008).…”

Section: Introductionmentioning

confidence: 99%

AnXMM-Newtonspatially-resolved study of metal abundance evolution in distant galaxy clusters

Baldi

Ettori

Molendi

et al. 2012

A&A

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Context. We present an XMM-Newton analysis of the X-ray spectra of 39 clusters of galaxies at 0.4 < z < 1.4, covering a temperature range of 1.5 < ∼ kT < ∼ 11 keV. Aims. The main goal of this paper is to study how the abundance evolves with redshift not only by means of a single emission measurement performed on the whole cluster but also by spatially resolving the cluster emission. Methods. We performed a spatially resolved spectral analysis, using Cash statistics and modeling the XMM-Newton background instead of subtracting it, by analyzing the contribution of the core emission to the observed metallicity. Results. We do not observe a statistically significant (>2σ) abundance evolution with redshift. The most significant deviation from no evolution (at a 90% confidence level) is observed by considering the emission from the whole cluster (r < 0.6r 500 ), which can be parametrized as Z ∝ (1 + z) −0.8±0.5 . Dividing the emission into three radial bins, no significant evidence of abundance evolution is observed when fitting the data with a power law. We find close agreement with measurements presented in previous studies. Computing the error-weighted mean of the spatially resolved abundances into three redshift bins, we find that it is consistent with being constant with redshift. Although the large error bars in the measurement of the weighted-mean abundance prevent us from claiming any statistically significant spatially resolved evolution, the trend with z in the 0.15-0.4r 500 radial bin complements nicely previous measurements and broadly agrees with theoretical predictions. We also find that the data points derived from the spatially resolved analysis are well-fitted by the relation Z(r, z) = Z 0 (1+ (r/0.15r 500 ) 2 ) −a ((1+ z)/1.6) −γ , where Z 0 = 0.36± 0.03, a = 0.32± 0.07, and γ = 0.25 ± 0.57, which represents a significant negative trend of Z with radius and no significant evolution with redshift. Conclusions. We present the first attempt to determine the evolution of abundance at different positions in the clusters and with redshift. However, the sample size and the low-quality data statistics associated with most of the clusters studied prevents us from drawing any statistically significant conclusion about the different evolutionary path that the different regions of the clusters may have traversed.

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“…Bruggen & Kaiser 2002;Omma et al 2004), the spreading of metals in the ICM (e.g. Schindler & Diaferio 2008;Borgani et al 2008), the stability of thermal profiles in the innermost region of galaxy clusters (e.g. Sharma et al 2009), the efficiency in the ram pressure stripping of accreting satellites and the emergence of cold fronts in galaxy clusters (e.g.…”

Section: Introductionmentioning

confidence: 99%

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

Vazza¹,

Gheller²,

Brunetti³

2010

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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 Chemical Enrichment of the ICM from Hydrodynamical Simulations

Cited by 61 publications

References 89 publications

On the Fe abundance peak formation in cool-core clusters of galaxies: hints from cluster WARPJ1415.1+3612 atz= 1.03

On the Fe abundance peak formation in cool-core clusters of galaxies: hints from cluster WARPJ1415.1+3612 atz= 1.03

AnXMM-Newtonspatially-resolved study of metal abundance evolution in distant galaxy clusters

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

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