The Three Hundred Project: The evolution of galaxy cluster density profiles

Robert Mostoghiu, Alexander Knebe, Weiguang Cui, Frazer R. Pearce, Gustavo Yepes, Chris Power, Romeel Dave, Alexander Arth

Research output: Contribution to journalArticle

Abstract

Recent numerical studies of the dark matter density profiles of massive galaxy clusters (M-halo > 10(15) M-circle dot) 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 themass-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 (similar to 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 similar to 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.

Original languageEnglish
Pages (from-to)3390-3403
Number of pages14
JournalMonthly Notices of the Royal Astronomical Society
Volume483
Issue number3
DOIs
Publication statusPublished - Mar 2019

Cite this

Mostoghiu, Robert ; Knebe, Alexander ; Cui, Weiguang ; Pearce, Frazer R. ; Yepes, Gustavo ; Power, Chris ; Dave, Romeel ; Arth, Alexander. / The Three Hundred Project : The evolution of galaxy cluster density profiles. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 483, No. 3. pp. 3390-3403.
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The Three Hundred Project : The evolution of galaxy cluster density profiles. / Mostoghiu, Robert; Knebe, Alexander; Cui, Weiguang; Pearce, Frazer R.; Yepes, Gustavo; Power, Chris; Dave, Romeel; Arth, Alexander.

In: Monthly Notices of the Royal Astronomical Society, Vol. 483, No. 3, 03.2019, p. 3390-3403.

Research output: Contribution to journalArticle

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

PY - 2019/3

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N2 - Recent numerical studies of the dark matter density profiles of massive galaxy clusters (M-halo > 10(15) M-circle dot) 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 themass-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 (similar to 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 similar to 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-circle dot) 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 themass-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 (similar to 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 similar to 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

KW - PARTICLE HYDRODYNAMICS SIMULATIONS

KW - COSMOLOGICAL SIMULATIONS

KW - DYNAMICAL STATE

KW - MATTER

KW - HALOES

KW - SCATTER

KW - MERGERS

KW - GROWTH

KW - INFALL

KW - MODEL

U2 - 10.1093/mnras/sty3306

DO - 10.1093/mnras/sty3306

M3 - Article

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 -