Collaborators within Collaborators within DK-DK-PlanckPlanck communitycommunity

Lung-Yih Chiang (NBI)Lung-Yih Chiang (NBI)

Andrei Doroshkevich (TAC,ASC FIRAN)

Per Rex Christensen (NBI)

Igor D. Novikov ( NBI)

Pavel D. Naselsky ( NBI)

Oleg V. Verhodanov(TAC,SAO RAN)

H..U Norgaard-Nielsen, DSRC

Non-Gaussianity of the CMB sky

P.NaselskyNBI, the PLANCK scientist

Why the issue of Why the issue of Non-Gaussianity Non-Gaussianity is important for is important for developmentdevelopmentof cosmology ?of cosmology ?

“BIG BANG”

Ω≈1 n≈0.97Gaussianity!!P(δ)dδ~exp(-δ ²/2σ²)dδ

Non-linear development of the quantum fluctuation

Non-Gaussianity!!

Transition from primordial (Gaussian) fluctuations to non-linear structures (galaxies , clusters and LSS ) change statistical properties of the adiabatic perturbations.

Picture of thePicture of theQuantum fluctuations fromQuantum fluctuations fromInflation in Inflation in radio wavesradio waves

Definition of the power spectraDefinition of the power spectra

)φ,(θY)iexp(|a|ΔT(θ,φ)

0 mmmm

2barm

mm

barm

|,......)n,,,(a|12

1

,......)n,,,(C

)2/1(f/1C/C

Gaussian or non-Gaussian

Gaussian only !

Cosmology before WMAP

The temperature anisotropy and temperature The temperature anisotropy and temperature

polarization cross power spectrumpolarization cross power spectrum

Precision cosmology !!!

BOOMERANG, MAXIMA-1,CBI,ARCHEOPS,VSA,DASI,BIMA +……. SN1a, 2dF,He,D…

CMB

Ω h =0.02 !b2

WMAP +……. SN1a, 2dF,He, D

WHY NOT FORNOT FORUS ?US ?

CosmologyCosmology ofof the XX centurythe XX century

Important question is WHY?Important question is WHY?

Dark matter densityDark energy density ≈1/3 1/π ? (D=3)/(D=10) ?

What about What about

ExtraExtra dimensions ?dimensions ?Topology ?Topology ?

Baryonic matter density Dark matter density ?Baryosynthesis?

CosmologyCosmology of the XXI centuryof the XXI century

Development of Development of Cosmology andCosmology andHigh energy physicsHigh energy physics

Dark energyDark energy

Dark matterDark matter

Baryonic matterBaryonic matter

}

ΦΦ(x, t)=(x, t)=ΨΨ(x, t)*(x, t)* exp [iexp [iΛΛ(x, t)](x, t)]

S.Bonometto et al,2004,2005

Non linear theory of dark energy-dark matterNon linear theory of dark energy-dark matter couplingcoupling

•Link between adiabatic and isocurvature perturbations•Weak Non-Gaussianity of the CMB

Reionization of the cosmic Reionization of the cosmic plasma by the first quasars, plasma by the first quasars, galaxies, and starsgalaxies, and stars

300 Mpc

3Mpc

ReionizationReionization

WMAPWMAP

PLANCK,PLANCK,20072007

Two news from the WMAP data analysisTwo news from the WMAP data analysis

1.The CMB signal is The CMB signal is Gaussian !Gaussian !

Komatsu et al, 2003 (WMAP teamteam ) )

2. The CMB signal is2. The CMB signal is non- Gaussiannon- Gaussian

WMAPWMAP map: Gaussian by map: Gaussian by WMAPWMAP science team with 95% CLscience team with 95% CL

f

f

, Non-Gaussianity is not a dog!” Non-Gaussianity is not a dog!” Ya.B.Zel’dovichYa.B.Zel’dovich

f*ΔΔΦΦΔΔΦΦ

The definition of Gaussianity

)iexp(|a|a mmm

dT]2

)TT(exp[NdT)T(P

2

2

Methods of detection of Non-Gaussianity in the WMAP sky

Image domain Multipoles domain

1.Peak statistics

2. Minkowski functionals

3. Wavelets

4.Curvature distribution

5.Non-uniformity of thepower spectra distributionover patches of the sky

6.Skiwness and kurtosis

7. Bispectrum

…………….

1.Phases analysis(trigonometric moments of phases, phase cross-correlations,Pearson’s random walk statistic,

2.Minkowski vectors

3. Cooper's statistic for phases

WMAP signalWMAP signal is Non-Gaussianis Non-Gaussian

FOREGROUNS +FOREGROUNS +instrumental noise+instrumental noise+systematic effectssystematic effects

CMB maps derived from the WMAP data

ILCl<100

FCM l<512

WFM l<512

ErFM l<512

NOT FORNOT FOR INVESTIGA-INVESTIGA-TION OF THETION OF THE CMB !!!??CMB !!!??

Image analysis for non-Gaussianity test

Pixel by pixel

Foregrounds ?

FCM-ErFCM ILC-ErFCM

ILC-WFM V band l=400

WMAP KP masksWMAP KP masks

Asymmetry of the CMB Asymmetry of the CMB powerpower

*South-north asymmetry of the *South-north asymmetry of the COBE and the WMAP signals.COBE and the WMAP signals.

Global anisotropy of the Universe.

NEP

NEP

SEP

SEP WHY ?

Non-CMB toolsNon-CMB toolsQ-W

V-W

FCM

WFCM

FCM-WFCM

MV

L<512

NON-CMB

L<100

L<30

Alignment of the low multipoles Schwarz et al,2004

Gaussian Random FieldsGaussian Random FieldsStrict definition of Gaussianity:

They possess Fourier modes whose real and imaginary parts are independently distributed and both Gaussian,

Weak definition of Gaussianity : random phase hypothesis

the Fourier phases are uniformly random between 0 and (by Central Limit Theorem)

]a[mi]a[)iexp(|a|a mmlmmm

transformed Planck

Planck satellite and transformed Planck have the same power spectrum (same |k| ), they have different “faces” due to different phases:It is phase k that keep Max’s face, not amplitude |k| !!

Planck satellite

Max Planck FT-1[ ]|k| exp(ik) |k| exp(ik)|k|exp(ik)

Asymmetry of the WMAP Asymmetry of the WMAP phasesphases

)cos()l(Cs

)sin()l(Si

})l(Cs

)l(Si{tan

1mm,llm

1

1mm,llm

1

1

Foreground-cleaned map

Foreground-cleaned map

ℓ

m

Asymmetry of the WMAP Asymmetry of the WMAP phasesphases

L-1,L+1 correlation through m- direction

M-1,M correlationthrough - L direction

ILC

WTOH

TOH

NO Evidence of Primordial Magnetic Field !Naselsky, Verkhodanov, Novikov,Olesen,Chiang,ApJ,2004

Non-Gaussianity of the WMAP.Non-Gaussianity of the WMAP.

WHY ?

Primordial(Inflation ?)

Foregrounds + systematic

NON-GAUSSIANITY

NEWPHYSICS

S= G + NG

f

Summary 2003-2005Summary 2003-20051.Residues of the foregrounds separation1.Residues of the foregrounds separationChiang ,Naselsky, Verkhodanov and Way,ApJ.Lett2003; Chiang ,Naselsky, Verkhodanov and Way,ApJ.Lett2003; Naselsky , Doroshkevich and Verkhodanov,ApJ.Lett,2003;Naselsky , Doroshkevich and Verkhodanov,ApJ.Lett,2003;Naselsky , Doroshkevich and Verkhodanov,MNRAS,2004;Naselsky , Doroshkevich and Verkhodanov,MNRAS,2004;Park, MNRAS,2004;Park, MNRAS,2004;Eriksen, D.Novikov, Lille,Gorski, ApJ,2004 ;Eriksen, D.Novikov, Lille,Gorski, ApJ,2004 ;Naselsky, Verkhodanov, Novikov,Olesen,Chiang,ApJ,2004,…Naselsky, Verkhodanov, Novikov,Olesen,Chiang,ApJ,2004,…

2. Systematic effects2. Systematic effectsHansen, Vittorio,ApJ.Lett.2004 (+)Hansen, Vittorio,ApJ.Lett.2004 (+)Vielva et al,MNRAS, 2004 (-)Vielva et al,MNRAS, 2004 (-)

3. Primordial3. PrimordialBershadskii, Skrinevasan, Phys.Lett.,2003;2004 (magnetic field)Bershadskii, Skrinevasan, Phys.Lett.,2003;2004 (magnetic field)Vielva et al,MNRAS, 2004 Vielva et al,MNRAS, 2004 Hansen, Bandy, Gorski,MNRAS,2004Hansen, Bandy, Gorski,MNRAS,2004Wandelt ,ApJ.Lett,2004Wandelt ,ApJ.Lett,2004

Non-Gaussianity is not a dog!” Non-Gaussianity is not a dog!” Ya.B.Zel’dovichYa.B.Zel’dovich

Sorry!