Combining cmb snia and weak lensing to study quitessence models work in progress
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Combining CMB, SnIa and weak lensing to study quitessence models work in progress. Carlo Schimd IAP  DAPNIA / CEA Saclay. I.Tereno, J.-P.Uzan, Y.Mellier, A.Riazuelo (IAP), L.vanWaerbeke (British Columbia Univ.). In collaboration with:.

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Combining CMB, SnIa and weak lensing to study quitessence models work in progress

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Combining CMB, SnIa and weak lensing to study quitessence modelswork in progress

Carlo Schimd

IAP  DAPNIA / CEA Saclay

I.Tereno, J.-P.Uzan, Y.Mellier, A.Riazuelo (IAP), L.vanWaerbeke (British Columbia Univ.)

In collaboration with:

December 2005 EDENINPARIS


Aim:low-z effects of quintessence

SNe + cosmic shear


Aim:low-z effects of quintessence

SNe + cosmic shear

2pts statistics

with respect to L , quintessence modify

  • angular distanceq(z); 3D2D projection

  • growth factor  amplitude of 3D L/NL power spectrum

     amplitude + shape of 2D spectra

20%

10%

z=1

K = 0


non-linear regime

  • N-body: ...

  • mappings: stable clustering, halo model, etc.:

e.g. Peacock & Dodds (1996)

Smith et al. (2002)

NLPm(k,z) = f[LPm(k,z)]

calibrated with LCDM N-body sim, 5-10% agreement

Huterer & Takada (2005)

 Ansatz: for every z we can use them, being dc, bias, c, etc. not so much dependent on cosmology

Q: dependence of 3D NL power spectrum on w ?

McDonald, Trac, Contaldi (2005)

  • normalization to high-z (CMB):

the modes k enter in non-linear regime ( s(k)1 ) at different time  3D non-linear power spectrum is modified  2D shear power spectrum is modified by

no more s8


pipeline

Boltzmann code

by A.Riazuelo

background dynamics

+ linear perturbations

in fCDM

*

*

w-lensing code

by C.S.

  • NNL mappings

  • 2pts statistics

  • tomography

Riazuelo & Uzan (2002)

C.S., Uzan & Riazuelo (2004)

*

SNe + cosmic shear

data analysis

*

grid method

  • Q models: inverse power law with/without SUGRA corrections

  • (restricted) parameter space:{WQ, a, ns, zsource}

  • fixed parameters: flat universe, h=0.72,Wbh2 =0.024, treion=0.17

*

They include larger framework: scalar-tensor theories of gravitation / extended quintessence models

*

CMB can be taken into account at no cost


dataset

  • CMB: TT anisotropy spectrum @ WMAP  initial conditions/

normalization

  • SNe: “goldset”

Riess et al. (2004)

VanWaerbeke, Mellier, Hoekstra (2004)

  • cosmic shear: VIRMOS-Descart

    +

    CFHTLS deep

Semboloni et al. (2005)

+ CFHTLS wide (sim)

Hoekstra et al. (2005): 22deg2

Fu’s talk

<z>  0.92, 1.0, 0.76

ngal  15, 23, 20 /arcmin2

area  8.5, 2.1, 170 deg2

wl observables: top-hat variance; aperture mass variance

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


deep survey : effects ofL-NL mapping

VIRMOS-Descart + CFHTLS deep

CFHTLS wide

*

*

*

ns

ns

ns

top-hat variance

WQ

WQ

WQ

low resolution effect. High-res in progress

ns

ns

ns

*

a

a

a

halo model

stable clustering

Smith et al. (2002)

Peacock & Dodds (1996)

 primordial universe (ns): because of high-z normalization, constraints strongly depend on L-NL mapping  NL regime (integrated effect)  wide angular scales are needed

 quintessence: no relevant differences due to L-NL mapping in deep surveys


wide survey : Q - geometrical effects

q > 20 arcmin

a

*

top-hat variance

WQ

WQ

WQ

q > 20 arcmin

ns

DE is more sensible to the geometrical factor

WQ

WQ

WQ

q > 20 arcmin

low resolution effect

ns

ns

ns

*

a

a

stable clustering

halo model

Peacock & Dodds (1996)

Smith et al. (2002)


cosmic shear + SNe : Q equation of state

CFHTLS wide

SNe “goldset”

Map2, Smith et al.

a

a

WQ

WQ

  • dynamical model of quintessence (scalar field):

    wQ = wQ(WQ, a) -- no parameterization e.g. à la Linder

  • comparison to parameterized models:

    translation (WQ, a)  wQ(z*), dwQ/da(z*) [z_pivot technique]


dark energy by Fisher matrix analysis

SNe

“goldset”

TT @ CMB

WMAP 1yr

CFHTLS wide:

top-hat variance; L-NL: Smith et al.

  • A= 170 deg2

  • ngal = 20/arcmin2

Remark: * = fiducial model

DUNE-like:

  • A= 20000 deg2

  • ngal = 35/arcmin2

Refregier’s talk


conclusions & prospects

  • quintessence at low-z by Sne + cosmic shear,using high-z informations (CMB/Cl normalization)

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

dynamical models of DE (not parameterization): fCDM

for the first time cosmic shear data to this task (Fu’s talk)

improvement: bigger parameter space

 1. combining also CMB data (high-z effects of DE);

2. MCMC analysis;

3. deviation from GR, e.g. EQ  wQ < -1

Martin, C.S., Uzan. (2005)

  • NL regime: L-NL mappings (caveat)

some parameters (nS) are sensible to L-NL mappings ( integrated effect ?), Q parameters feel only geometry

 wide field surveys are needed  DUNE (Refregier’s talk)

Work in progress:

  • analysis of realistic (=dynamical) models of DE using severalparameters

other techniques: cross-correlations, tomography

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


Thank you


...DUNE : Fisher matrix analysis

WMAP 1yr

+

  • CFHTLS wide:

  • A= 170 deg2

  • ngal = 20/arcmin2

  • DUNE:

  • A= 20000 deg2

  • ngal = 35/arcmin2

top-hat variance; L-NL: Smith et al


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