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 models work in progress

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


Combining cmb snia and weak lensing to study quitessence models work in progress

Aim:low-z effects of quintessence

SNe + cosmic shear


Combining cmb snia and weak lensing to study quitessence models work in progress

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


Combining cmb snia and weak lensing to study quitessence models work in progress

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


Combining cmb snia and weak lensing to study quitessence models work in progress

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


Combining cmb snia and weak lensing to study quitessence models work in progress

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


Combining cmb snia and weak lensing to study quitessence models work in progress

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


Combining cmb snia and weak lensing to study quitessence models work in progress

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)


Combining cmb snia and weak lensing to study quitessence models work in progress

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]


Combining cmb snia and weak lensing to study quitessence models work in progress

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


Combining cmb snia and weak lensing to study quitessence models work in progress

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


Combining cmb snia and weak lensing to study quitessence models work in progress

Thank you


Combining cmb snia and weak lensing to study quitessence models work in progress

...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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