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

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....

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

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.

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

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

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.

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?

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

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∆

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

DEUSSIMULATIONS:

IMPRINTS OF DARKENERGY ON THE

PROFILE OF DARKMATTER HALOS

IRÈNE BALMÈS