deus simulations: imprints of dark energy on the profile
TRANSCRIPT
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
DEUS SIMULATIONS: IMPRINTS OF DARK
ENERGY ON THE PROFILE OF DARK
MATTER HALOS
Irène BALMÈS
part of the DEUS team including Jean-Michel ALIMI,Pier-Stefano CORASANITI, Yann RASERA, Vincent
BOUILLOT, Vincent REVERDY, Linda BLOT...
COSMO 2013September 3rd 2013
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
Balmès, Rasera, Corasaniti & Alimi, arXiv:1307.2922
NAVARRO, FRENK AND WHITE PROFILE
Phenomenological density profile from the simulations
ρ(r) =ρs
rrs
(1 + rrs
)2
concentration: c = r200rs
How does c evolve with mass?
VAST LITERATURE
Navarro et al. 1997, Bullock et al. 2001, Zhao et al. 2003,2009, Dolag et al. 2004....
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
1 NUMERICAL SET-UP
2 CONCENTRATION
3 SPARSITY
4 PROSPECTS
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
DEUS SIMULATIONS
I multiple box-sizes andresolutions
I large mass rangeI several cosmological models
see www.deus-consortium.org
Ideal set-up to study imprints of cosmology on non-linearstructure formation, and in particular on halo profiles.
In this study, (mostly) box of 162 Mpc and Npart = 5123.
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
HALO FINDER
Spherical OverDensity (SOD)Friend of Friend (FoF)
For each halo we obtain: M200, r200, c, χ2
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
NUMERICAL EFFECTS ON χ2
Renormalization: χ2 = χ2/√
npartχ2 independent of the resolution
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
3 HALO GROUPS
I Halos fitted towithin 1σ: 68 %
I Halos fitted towithin 2σ: 95 %
I Halos ill-fitted: 5%
χ2 limits vary with cosmology and redshift.
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
Great variations among the different groups. Find a morestable parameter?
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
SPARSITY
s∆ =M200
M∆
I no fittingrequired
I (nearly)independentof the halomass
⇒ Consistency relation between s∆ and the massfunctions∫
1M∆
dnd ln M∆
d ln M∆ = s∆
∫1
M200
dnd ln M200
d ln M200
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
VARIATION WITH THE COSMOLOGYOF s∆ pink: ΩΛ = 0
blue: ΩΛ = 0.9grey: toy-modelRatra-Peeblescyan: realisticRatra-Peeblesviolet:ΛCDM-WMAP3orange:SuperGravity
Cosmological variations linked to σ8 and D+
I the higher D+, the lower s∆
I the higher σ8, the lower s∆
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS
NUMERICALSET-UP
CONCENTRATION
SPARSITY
PROSPECTS
I confrontation to observations
I 2D sparsity
I DEUS FUR data
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DEUSSIMULATIONS:
IMPRINTS OF DARKENERGY ON THE
PROFILE OF DARKMATTER HALOS
IRÈNE BALMÈS