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Tracking quintessence by cosmic shear constraints from VIRMOS-Descart and CFHTLS and future...
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Transcript of Tracking quintessence by cosmic shear constraints from VIRMOS-Descart and CFHTLS and future...
Tracking quintessence by cosmic shearTracking quintessence by cosmic shear
constraints from VIRMOS-Descart and constraints from VIRMOS-Descart and CFHTLS and future prospectsCFHTLS and future prospects
May 2006 workshop PNC – IPNL Lyon
In collaboration with: I.Tereno, J.-P.Uzan, Y.Mellier, (IAP), L.vanWaerbeke (British Columbia U.), ...
Carlo SchimdCarlo Schimd
DAPNIA / CEA Saclay & IAPDAPNIA / CEA Saclay & IAP
Based on: astro-ph/0603158astro-ph/0603158
Dark energy:Dark energy: parametrization .vs. field theory inspired parametrization .vs. field theory inspired
{baryons,{baryons,,,}} + DM + GR + DM + GR alone cannot account for the cosmological dynamics seen by CMB + LSS + SNe + ...
GR : not valid anymore?
Other “matter” fields? Cosmological constant?
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)
Which class ?Which class ?
Physics-inspired approach:Physics-inspired approach:
high-energy physics ?!
w : full redshift range
small # p.
perturbations: consistently accounted for
Uzan, Aghanim, Mellier (2004); Uzan, astro-ph/0605313
scalar field quintessence:scalar field quintessence: models models
CMB
SNe, WL, n(z)
4( ) /V M 4 21
2( ) / exp( )V M
Inverse power law (Ratra-Peebles):
» + SUGRA corr. :
1 p. 1 p.
SU
GR
A
by-product: w(z) and w’(z) at whatever pivot redshift (zp)
zp = 0 zp = 0.5
w
w’
0.01 0.1 1 10 100 1000
0.00
0.05
0.10
0.15
0.20
0.25
0.30
= 6
= 11
= 6
= 11
z = 3.43
z = 4.75
QC
DM
/ C
DM
redshift
RP SUGRA
quintessence by cosmic shearquintessence by cosmic shear
angular distanceangular distance q(z); 3D2D projection growth factor growth factor amplitude of 3D L/NL power spectrum
amplitude + shape of 2D spectra
with respect to , quintessence modifies
2pts statistics 2( ) ( ) ,( )
m
K
P dz q z P k zS z
z=1
10%
20%
K = 0
cosmic shear = cosmic shear =
weak lensing by LSSweak lensing by LSS
obs
gal
statistics, e.g.
0.01 0.1 1 10 100 10000.4
0.5
0.6
0.7
0.8
0.9
1.0
= 6 = 11
d ln
D+
/ d ln
a
redshift
CDM SUGRA RP
non-linear regime non-linear regime
N-body:N-body: ... mappings:mappings: stable clustering, halo model, etc.:
NLPm(k,z) = f[LPm(k,z)]
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)
no more ,but incertitude on TT-CMB Cl’s
e.g. Peacock & Dodds (1996) Smith et al. (2003)
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)...
calibrated with CDM N-body sim, 5-10% agreementHuterer & Takada (2005)
Q:Q: dependence of 3D NL power spectrum on wQ ? McDonald, Trac, Contaldi (2005)
pipelinepipeline
**
Ria
zuelo
& U
zan (
2002
)C
.S., U
z an &
Ria
zuelo
(2
004)
* They include larger framework: scalar-tensor theories of gravitation / extended Q models
* CMB can be taken into account at no cost
Q models:Q models: inverse power law with/without SUGRA corrections
(restricted) parameter space:(restricted) parameter space:Q, , ns, zsource; marginalization over zsource
* *
*
*
*
datasetdataset
CMB:CMB: TT anisotropy spectrum @ WMAP-1yr initial conditions/
SNe:SNe: “goldset”
cosmic shear:cosmic shear: VIRMOS-Descart +
CFHTLS deep
VanWaerbeke, Mellier, Hoekstra (2004)
Semboloni et al. (2005)
+ CFHTLS wide/22deg2 & 170deg2 (synth)
<z> 0.92, 1.0, 0.76 ngal 15, 22, 20 /arcmin2
area 8.5, 2.2, 22(170) deg2
IAB 24.5, 26, 26
0 1 2 3 4 50.0
0.5
1.0
z
p(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
cosmic shear data*:cosmic shear data*: effects of effects of L-NLL-NL mapping mappingR
atr
a-P
eeble
sSU
GR
A
** Joint VIRMOS-Descart + CFHTLS deep + CFHTLS wide/22deg2 analysis
Peacock & Dodds (1996)
Smith et al. (2003)
Top-hat shear variance
Peacock & Dodds
Smith et al.
wide survey :wide survey : Q - geometrical effects (RP) Q - geometrical effects (RP)R
atr
a-P
eeble
s
Peacock & Dodds (1996)
CFHTLS wide/22deg2 (real datareal data)
CFHTLS wide/170deg2 (synthsynth)
CFHTLS wide/170deg2 (synthsynth)
top-hattop-hat variance
top-hattop-hat variance
aperture mass aperture mass variancevariance
only scales > 20 arcmin> 20 arcmin
CFHTLS wide/170deg2 (synthsynth)
top-hattop-hat variance
wide survey :wide survey : Q - geometrical effects (SUGRA) Q - geometrical effects (SUGRA)SU
GR
A
Peacock & Dodds (1996)
CFHTLS wide/22deg2 (real datareal data)
CFHTLS wide/170deg2 (synthsynth)
CFHTLS wide/170deg2 (synthsynth)
top-hattop-hat variance
top-hattop-hat variance
aperture mass aperture mass variancevariance
only scales > 20 arcmin> 20 arcmin
CFHTLS wide/170deg2 (synthsynth)
top-hattop-hat variance
cosmic shear alone :cosmic shear alone : summary summary
Two classes of cosmological parameters:Two classes of cosmological parameters:
other parameters:other parameters: sensible to L-NL mapping
Q parameters:Q parameters: not sensible to linear-to-nonlinear mapping
This conclusions holds for both Ratra-Peebles and SUGRA modelsThis conclusions holds for both Ratra-Peebles and SUGRA models
real data (VIRMOS-Descart + CFHTLS deep + CFHTLS wide/22deg2)
synthetic data (CFHTLS wide/170deg2)
Confirmation of results based on real data joint Confirmation of results based on real data joint analysisanalysis
Based on top-hat shear variance measurementsBased on top-hat shear variance measurements
Agreement top-hat shear variance – aperture mass varianceAgreement top-hat shear variance – aperture mass variance
Compatible with CDM (=0), towards ns=0.95 (like WMAP3!)
Analysis of wide scale Analysis of wide scale reducing the non-linear contamination reducing the non-linear contamination
confirming Simpson & Bridle (2005)
cosmic shear + SNe cosmic shear + SNe + CMB+ CMB:: Q equation of state Q equation of state
Ratra-Peebles SUGRA
(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):
• RP: RP: strong degeneracy with SNe
• SUGRA:SUGRA:
1) beware of systematics! (wl: calibration when combining datasets)
2) limit case: prefectly known/excluded Q model (weakly -dependece)
Van Waerbeke et al. (2006)
cosmic shear & CMB:cosmic shear & CMB: variance on 8 variance on 8hh-1-1 Mpc ( Mpc (88) )
contours follow 8 degeneracy
WMAP3 – weak lensing:WMAP3 – weak lensing: stress{h,reion,normalization,q}
Ratr
a-P
eeble
sSU
GR
A
Spergel et al. 2006
Check normalization procedure
Check calibration of datasets
Deviations from CDM ?
-1.75 -1.5 -1.25 -1 -0.75 -0.5
0.1
0.2
0.3
0.4
0.5
a remark on constant a remark on constant ww
zde
zacc
de/m = 0.6/0.4
Spergel et al. 2006Hoekstra et al. 2006 Astier et al. 2005
( ) ( )de demde z z
( ) 0accza
,03
,0
,03
,0
(1 )
1(1 )
1 3
dew
m
dew
macc
de
zw
z
w = const
Q by cosmic shear:Q by cosmic shear: Fisher matrix analysis Fisher matrix analysis
CFHTLSCFHTLSwide/170wide/170
SNAPSNAP
Like previous data analysis:Like previous data analysis: all but (,q,ns) fixed, zs marginalized
SNAPSNAP
DUNEDUNE
CFHTLSCFHTLSwide/170wide/170
DUNEDUNE
Adding a parameter:Adding a parameter: Like upper plots but reion marginalized size, orientation
conclusions & prospects conclusions & prospects
quintessence at low-z quintessence at low-z by SNe + cosmic shear, using high-z informations (TT-CMB/Cl normalization)
dynamical models of DE (not parameterization): CDMCDM
wide field surveyswide field surveys are needed DUNE, LSST
for the first time cosmic shear datadata to this task improvement:improvement: bigger parameter space 1.1. combining also CMB data (high-z effects of DE) + ... ;
2.2. MCMC analysis;
3.3. deviation from GR, e.g. EQ wQ < -1
NL regime:NL regime: L-NL mappings (caveatcaveat)
Martin, C.S., Uzan (2005)
some parameters (nS) are sensible to L-NL mappings ( integrated effect ?), Q parameters feel only geometry
Tereno et al. (2005)
deep surveysdeep surveys help to exploit the linear regime SKASchneider (1999);Chang, Réfrégier, Helfand
(2004)
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