Abstract
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.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 3390-3403 |
| Number of pages | 14 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 483 |
| Issue number | 3 |
| DOIs | |
| State | Published - Jan 1 2019 |
| Externally published | Yes |
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Keywords
- cosmology theory
- Dark matter
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
Cite this
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 S; Arth, Alexander.
In: Monthly Notices of the Royal Astronomical Society, Vol. 483, No. 3, 01.01.2019, p. 3390-3403.Research output: Contribution to journal › Article
}
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 S
AU - Arth, Alexander
PY - 2019/1/1
Y1 - 2019/1/1
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 - cosmology theory
KW - Dark matter
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
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 -