TY - JOUR
T1 - The Three Hundred Project
T2 - The evolution of galaxy cluster density profiles
AU - Mostoghiu, Robert
AU - Knebe, Alexander
AU - Cui, Weiguang
AU - Pearce, Frazer R.
AU - Yepes, Gustavo
AU - Power, Chris
AU - Dave, Romeel
AU - Arth, Alexander
N1 - Funding Information:
The work has received financial support from the European Union’s Horizon 2020 Research and Innovation programme under the Marie Sklodowskaw-Curie grant agreement number 734374, i.e. the LACEGAL project.7 The workshop where this work has been finished was sponsored in part by the Higgs Centre for Theoretical Physics at the University of Edinburgh.
Funding Information:
RM, AK, WC, and GY are supported by the Ministerio de Economía y Competitividad and the Fondo Europeo de Desar-rollo Regional (MINECO/FEDER, UE) in Spain through grant AYA2015-63810-P. AK is also supported by the Spanish Red Con-solider MultiDark FPA2017-90566-REDC and further thanks The Perishers for let there be morning. CP acknowledges the Australia Research Council (ARC) Centre of Excellence (CoE) ASTRO 3D through project number CE170100013. The authors would like to thank The Red Española de Supercomputación for granting us computing time at the MareNostrum Supercomputer of the BSC-CNS where most of the cluster simulations have been performed. Part of the computations with GADGET-X have also been performed at the ‘Leibniz-Rechenzentrum’ with CPU time assigned to the Project ‘pr83li’.
PY - 2019
Y1 - 2019
N2 - Recent numerical studies of the dark matter density profiles of massive galaxy clusters (M halo > 10 15 M) show that their median radial mass density profile remains unchanged up to z > 1, displaying a highly self-similar evolution. We verify this by using the data set of the THE THREE HUNDRED project, i.e. 324 cluster-sized haloes as found in full physics hydrodynamical simulations. We track the progenitors of the mass-complete sample of clusters at z = 0, and find that their median shape is already in place by z = 2.5. However, selecting a dynamically relaxed subsample (∼16 per cent of the clusters), we observe a shift of the scale radius r s towards larger values at earlier times. Classifying the whole sample by formation time, this evolution is understood as a result of a two-phase halo mass accretion process. Early-forming clusters – identified as relaxed today – have already entered their slow accretion phase, hence their mass growth occurs mostly at the outskirts. Late-forming clusters – which are still unrelaxed today – are in their fast accretion phase, thus the central region of the clusters is still growing. We conclude that the density profile of galaxy clusters shows a profound self-similarity out to redshifts z ∼ 2.5. This result holds for both gas and total density profiles when including baryonic physics, as reported here for two rather distinct sub-grid models.
AB - Recent numerical studies of the dark matter density profiles of massive galaxy clusters (M halo > 10 15 M) show that their median radial mass density profile remains unchanged up to z > 1, displaying a highly self-similar evolution. We verify this by using the data set of the THE THREE HUNDRED project, i.e. 324 cluster-sized haloes as found in full physics hydrodynamical simulations. We track the progenitors of the mass-complete sample of clusters at z = 0, and find that their median shape is already in place by z = 2.5. However, selecting a dynamically relaxed subsample (∼16 per cent of the clusters), we observe a shift of the scale radius r s towards larger values at earlier times. Classifying the whole sample by formation time, this evolution is understood as a result of a two-phase halo mass accretion process. Early-forming clusters – identified as relaxed today – have already entered their slow accretion phase, hence their mass growth occurs mostly at the outskirts. Late-forming clusters – which are still unrelaxed today – are in their fast accretion phase, thus the central region of the clusters is still growing. We conclude that the density profile of galaxy clusters shows a profound self-similarity out to redshifts z ∼ 2.5. This result holds for both gas and total density profiles when including baryonic physics, as reported here for two rather distinct sub-grid models.
KW - Dark matter
KW - cosmology theory
UR - http://www.scopus.com/inward/record.url?scp=85063620191&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85063620191&partnerID=8YFLogxK
U2 - 10.1093/mnras/sty3306
DO - 10.1093/mnras/sty3306
M3 - Article
AN - SCOPUS:85063620191
VL - 483
SP - 3390
EP - 3403
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 3
ER -