Scalar field quintessence by cosmic shear constraints from VIRMOS-Descart and CFHTLS and future prospects July 2006, Barcelona IRGAC 2006 In collaboration

Scalar field quintessence by cosmic shearScalar field quintessence by cosmic shear

constraints from VIRMOS-Descart and CFHTLS constraints from VIRMOS-Descart and CFHTLS and future prospectsand future prospects

July 2006, Barcelona IRGAC 2006

In collaboration with: I.Tereno, J.-P.Uzan, Y.Mellier, (IAP), L.vanWaerbeke (British Columbia U.), ...

Carlo SchimdCarlo Schimd

DAPNIA / CEA Saclay DAPNIA / CEA Saclay @ @ DUNE TeamDUNE Team

& Institut d’Astrophysique de Paris& Institut d’Astrophysique de Paris

Based on: astro-ph/0603158astro-ph/0603158

Dark energy:Dark energy: parametrization .vs. “physics” inspired parametrization .vs. “physics” inspired

{baryons,{baryons,,,}} + DM + GR + DM + GR alone cannot account for the cosmological dynamics seen by CMB + LSS + SNe + ...

GR : not valid anymore? scalar-tensor theories, braneworld, etc.

Other “matter” fields? cosmological constant, quintessence, K-essence, etc.

Dark energyDark energy H(z)-Hr+m+GR(z)

1/0 approach:1/0 approach: parameterization of w(z) departures from CDM

limitation in redshift ?pivot redshift zp : observable/dataset dependent

Not adapted for combining low-z and high-z observables and/or several datasets

parameters physics# p.: limitation to likelihood computation

perturbations: how ? Fitted T(k)

Physics-inspired approach:Physics-inspired approach: classes experimental/observational tests

high-energy physics ?!

w : full redshift range small # p.perturbations: consistently accounted for

Validity of Copernican principle? effect of inhomogeneities?

geodesic deviation equation

Quintessence by cosmic shear. IQuintessence by cosmic shear. I

convergence shear

2 4

( )

( ) ( ) ( ) ,K

k S

P P d q k P k

N-pts 2-pts correlation functions in real space:(0) ( )

Remark: just geometry, valid also for ST gravity

i i ji ijB v E v v

2 2 2( ) (1 2 ) ((1 2 ) 2 )i ii i j

ij jds a d d dx x dxB dE

C.S., J.-P.Uzan, A.Riazuelo (2004)

( ) ( )Pd W

obs

gal

1 22 2 2 21 2 1 2 1 2 2 1

LSS:

Map

2

v i

angular distanceangular distance q(z); 3D2D projectiongrowth factor growth factor amplitude of 3D L/NL power spectrum

amplitude + shape of 2D spectra

with respect to , quintessence modifies

Quintessence by cosmic shear. IIQuintessence by cosmic shear. II

2( ) ( ) ,( )

m

K

P dz q z P k zS z

( ) ( ), [ ( )]Kq z n z S z

NON-LINEAR regime:NON-LINEAR regime: N-body:N-body: ... mappings:mappings: stable clustering, halo model, etc.:

NLPm(k,z) = f[LPm(k,z)] e.g. Peacock & Dodds (1996) Smith et al. (2003)calibrated with CDM N-body sim, 5-10% agreementHuterer & Takada (2005)

QCDM QCDM GR GR

Poisson eq.

2

2

( )( , ) ( , )

( )

LIN LINm m lss

lss

D zP k z P k z

D z

...normalization to high-z (CMB):normalization to high-z (CMB):

the modes k enter in non-linear regime ( (k)1 ) at different time 3D non-linear power spectrum is modified 2D shear power spectrum is modified by k = / SK (z)

Ansatz:Ansatz: c, bias, c, etc. not so much dependent on cosmology at every z we can use them, provided we use the correct linear growth factor (defining the onset of the NL regime)...

**

Ria

zuelo

& U

zan (

2002

)C

.S., U

z an &

Ria

zuelo

(2

004)

*

* CMB can be taken into account at no cost

Q models:Q models: self-interacting scalar fieldminimally/non-minimally couled to g

* *

*

pipelinepipeline

no fit for power spectrano fit for power spectra

(restricted) parameter space:(restricted) parameter space:Q, , ns, zsource; marginalization over zsource

4( ) /V M 4 212( ) / exp( )V M

0 1 2 3 4 50.0

0.5

1.0

z

n(z) VIRMOS

deep wide

wide surveywide survey :: Q - geometrical effects (IPL) Q - geometrical effects (IPL)inverse power law

Peacock & Dodds (1996)

CFHTLS wide/22deg2 (real datareal data)

CFHTLS wide/170deg2 (synthsynth)


top-hattop-hat variance


aperture mass aperture mass variancevariance

only scales > 20 arcmin> 20 arcmin



wide survey wide survey :: Q - geometrical effects (SUGRA) Q - geometrical effects (SUGRA)SUGRA

Peacock & Dodds (1996)

CFHTLS wide/22deg2 (real datareal data)





aperture mass aperture mass variancevariance

only scales > 20 arcmin> 20 arcmin



cosmic shear + SNecosmic shear + SNe + CMB+ CMB : Q equation of state : Q equation of state

inverse power lawinverse power law SUGRASUGRA

(ns,zs): marginalized ; all other parameters: fixed

SNe: confirmed literature

TT-CMB: rejection from first peak (analytical (Doran et al. 2000) & numerical)

Mass scale M: indicative

Cosmic shearCosmic shear (real data only):

• IPL: IPL: strong degeneracy with SNe

• SUGRA:SUGRA:

1) beware of systematics! (wl: calibration when combining datasets)

2) limit case: prefectly known/excluded Q model (weakly -dependence)

Van Waerbeke et al. (2006)

VIRMOS-Descart + CFHTLS deep + CFHTLS wide/22deg2 + “goldset”@SNe

Q by cosmic shear Q by cosmic shear : Fisher matrix analysis: Fisher matrix analysis

CFHTLSCFHTLSwide/170wide/170

DUNEDUNE

= real data analysis += real data analysis + reion :: all but (,q,ns) fixed, (reion,zs) marginalized

inverse-power lawinverse-power law

SNeSNe“goldset”

CFHTLSCFHTLSwide/170wide/170

TT @ CMBTT @ CMBWMAP 1yr

•A = 170 deg2

•ngal = 20/arcmin2

SUGRASUGRA

DUNE (pi: A.Réfrégier):DUNE (pi: A.Réfrégier):

wide, shallow surveyoptimized for WL + SNe

• A= 20000 deg2

• ngal = 35/arcmin2

All but (,q) fixed

inverse-power lawinverse-power law

present setup:

conclusions & prospects conclusions & prospects

quintessence at low-zquintessence at low-z by SNe + cosmic shear, using high-z informations (TT-CMB/Cl normalization)

dynamical models of DE (not parameterization): CDMCDM

wide, shallow cosmic shear surveyswide, shallow cosmic shear surveys are suitable

for the first time cosmic shear datadata to this task

NL regime:NL regime: (two) L-NL mappings (caveatcaveat)

Q parameters (seem to) feel only geometry

consistent joint analysis of high-z (CMB) and low-z (cosmic shear, Sne,...) observables no stress between datasets; no pivot redshift

analysisanalysis of realistic (=dynamical) models of DE using severalseveral parametersparameters

other techniquesother techniques: cross-correlations (ISW), 3pts functions, tomography

Work in progress:Work in progress:

pipeline: pipeline: Boltzmann code + lensing code + data analysis by grid method:

in collaboration with: I.Tereno, Y.Mellier , J.-P. Uzan, R. Lehoucq, A. Réfrégier & DUNE team

1.1. + CMB data; 2.2. MCMC analysis (Tereno et al. 2005)

astro-ph/0603158astro-ph/0603158

Thank youThank you

CMB:CMB: TT anisotropy spectrum @ WMAP-1yr initial conditions/

SNe:SNe: “goldset”

cosmic shear:cosmic shear: VIRMOS-Descart VanWaerbeke, Mellier, Hoekstra (2004)Semboloni et al. (2005)

CFHTLS wide/22deg2 & 170deg2 (synth)

0 1 2 3 4 50.0

0.5

1.0

z

n(z) VIRMOS

deep wide

wl observables:wl observables: top-hat variance; aperture mass variance

Riess et al. (2004)

cosmic shear:cosmic shear: by wide-field imager/DUNE-like satellite mission

Hoekstra et al. (2005)

normalization

CFHTLS deep

Q models, datasets & likelihood analysisQ models, datasets & likelihood analysis

(restricted) parameter space:(restricted) parameter space:Q, , ns, zsource; marginalization over zsource

Q models:Q models:

2( ) ( ) ( , )U U d U

/

4( ) /V M 4 212( ) / exp( )V M ;;

Documents

Scalar field quintessence by cosmic shear constraints from VIRMOS-Descart and CFHTLS and future prospects July 2006, Barcelona IRGAC 2006 In collaboration