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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/29279
Title: The origin of ICM enrichment in the outskirts of present-day galaxy clusters from cosmological hydrodynamical simulations
Authors: Biffi, V.
Planelles, S.
BORGANI, STEFANO 
RASIA, ELENA 
MURANTE, Giuseppe 
Fabjan, D.
GASPARI, MASSIMO 
Issue Date: 2018
Journal: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 
Number: 476
Issue: 2
First Page: 2689
Abstract: The uniformity of the intracluster medium (ICM) enrichment level in the outskirts of nearby galaxy clusters suggests that chemical elements were deposited and widely spread into the intergalactic medium before the cluster formation. This observational evidence is supported by numerical findings from cosmological hydrodynamical simulations, as presented in Biffi et al., including the effect of thermal feedback from active galactic nuclei. Here, we further investigate this picture, by tracing back in time the spatial origin and metallicity evolution of the gas residing at z = 0 in the outskirts of simulated galaxy clusters. In these regions, we find a large distribution of iron abundances, including a component of highly enriched gas, already present at z = 2. At z > 1, the gas in the present-day outskirts was distributed over tens of virial radii from the main cluster and had been already enriched within high-redshift haloes. At z = 2, about 40 {per cent} of the most Fe-rich gas at z = 0 was not residing in any halo more massive than 10^{11} h^{-1} M_{☉} in the region and yet its average iron abundance was already 0.4, w.r.t. the solar value by Anders & Grevesse. This confirms that the in situ enrichment of the ICM in the outskirts of present-day clusters does not play a significant role, and its uniform metal abundance is rather the consequence of the accretion of both low-metallicity and pre-enriched (at z > 2) gas, from the diffuse component and through merging substructures. These findings do not depend on the mass of the cluster nor on its core properties.
URI: http://hdl.handle.net/20.500.12386/29279
URL: http://arxiv.org/abs/1801.05425v2
https://academic.oup.com/mnras/article-abstract/476/2/2689/4850653?redirectedFrom=fulltext
ISSN: 0035-8711
DOI: 10.1093/mnras/sty363
Bibcode ADS: 2018MNRAS.476.2689B
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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