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This work has been made possible by THE THREEHUNDRED collaboration,6 which benefits from financial support of the European Union's Horizon 2020 Research and Innovation programme under the Marie Sklodowska-Curie Actions grant agreement number 734374, i.e. the LACEGAL project. THE THREEHUNDRED simulations used in this paper have been performed in the MareNostrum Supercomputer at the Barcelona Supercomputing Center because of CPU time granted by the Red Espanola de Supercomputacion. UK acknowledges support from STFC. GY and AK acknowledge financial support from Ministerio de Ciencia, Innovacion y Universidades/Fondo Europeo de Desarrollo Regional, under research grant PGC2018-094975-C21. WC acknowledges support from the European Research Council under grant number 670193 (the COSFORM project). FS and AR acknowledge the financial support from Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET, Argentina) by PICT-2016-4174 grant and Secretaria de Ciencia y Tecnologia de la Universidad Nacional de Cordoba (SeCyT, UNC, Argentina) by Consolidar-2018-2020 grant.

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THE THREEHUNDRED: the structure and properties of cosmic filaments in the outskirts of galaxy clusters

Publicado en:MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 502 (1): 714-727 - 2021-03-01 502(1), DOI: 10.1093/mnras/staa3792

Autores: Rost, Agustin; Kuchner, Ulrike; Welker, Charlotte; Pearce, Frazer; Stasyszyn, Federico; Gray, Meghan; Cui, Weiguang; Dave, Romeel; Knebe, Alexander; Yepes, Gustavo; Rasia, Elena;

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Galaxy cluster outskirts are described by complex velocity fields induced by diffuse material collapsing towards filaments, gas, and galaxies falling into clusters, and gas shock processes triggered by substructures. A simple scenario that describes the large-scale tidal fields of the cosmic web is not able to fully account for this variety, nor for the differences between gas and collisionless dark matter. We have studied the filamentary structure in zoom-in resimulations centred on 324 clusters from THE THREEHUNDRED project, focusing on differences between dark and baryonic matter. This paper describes the properties of filaments around clusters out to five R-200, based on the diffuse filament medium where haloes had been removed. For this, we stack the remaining particles of all simulated volumes to calculate the average profiles of dark matter and gas filaments. We find that filaments increase their thickness closer to nodes and detect signatures of gas turbulence at a distance of similar to 2 h(-1) from the cluster. These are absent in dark matter. Both gas and dark matter collapse towards filament spines at a rate of similar to 200 km s(-1) h(-1). We see that gas preferentially enters the cluster as part of filaments, and leaves the cluster centre outside filaments. We further see evidence for an accretion shock just outside the cluster. For dark matter, this preference is less obvious. We argue that this difference is related to the turbulent environment. This indicates that filaments act as highways to fuel the inner regions of clusters with gas and galaxies.

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