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Collaborators within DK- Planck community

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Collaborators within DK-Planckcommunity

Lung-Yih Chiang (NBI)

Andrei Doroshkevich

(TAC,ASC FIRAN)

Per Rex

Christensen (NBI)

Igor D. Novikov ( NBI)

H..U Norgaard

-Nielsen, DSRC

Oleg V. Verhodanov

(TAC,SAO RAN)

Pavel D. Naselsky ( NBI)

Non-Gaussianity

is important for

development

of cosmology ?

Non-Gaussianity of the CMB sky

P.Naselsky

NBI, the PLANCK scientist

Ω≈1 n≈0.97

Gaussianity!!

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 the non-linear structures (galaxies , clusters and LSS ) change statistical properties of the adiabatic perturbations.

Quantum fluctuations from

Inflation in radio waves

Definition of the power spectra non-linear structures (galaxies , clusters and LSS ) change statistical properties of the adiabatic perturbations.

Gaussian or

non-Gaussian

Gaussian only !

Cosmology before WMAP non-linear structures (galaxies , clusters and LSS ) change statistical properties of the adiabatic perturbations.

The temperature anisotropy and temperature polarization cross power spectrum

Precision

cosmology !!!

WMAP cross power spectrum+……. SN1a,2dF,He, D

BOOMERANG, MAXIMA-1,CBI,ARCHEOPS,VSA,DASI,

BIMA +……. SN1a,2dF,He,D…

CMB

Ω h =0.02 !

2

b

WHY

NOT FOR

US ?

Cosmologyof

the XX century

Cosmology cross power spectrumof the XXI century

Important question is WHY?

1/π ?

(D=3)/(D=10) ?

Dark matter density

Dark energy density

≈1/3

Extradimensions ?

Topology ?

?

What about

Baryosynthesis?

Baryonic matter density

Dark matter density

Dark energy cross power spectrum

}

Development of

Cosmology and

High energy physics

Dark matter

Φ(x, t)=Ψ(x, t)*

exp [iΛ(x, t)]

Baryonic matter

S.Bonometto et al,2004,2005

Non linear theory of dark energy-dark matter cross power spectrum

coupling

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

Reionization of the cosmic

plasma by the first quasars,

galaxies, and stars

Two news from the WMAP data analysis cross power spectrum

- The CMB signal is
- Gaussian !

Komatsu et al, 2003 (WMAP team )

2. The CMB signal is

non- Gaussian

WMAP cross power spectrum map: Gaussian by WMAP science team with 95% CL

!

?

|f |<100

Df = DF + f *DF*DF

The definition of Gaussianity cross power spectrum

Methods of detection of Non-Gaussianity in the WMAP sky cross power spectrum

Image domain

Multipoles domain

1.Peak statistics

2. Minkowski functionals

3. Wavelets

4.Curvature distribution

5.Non-uniformity of the

power spectra distribution

over 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 signal

is Non-Gaussian

CMB maps derived from the WMAP data cross power spectrum

NOT FOR

INVESTIGA-

TION OF THE

CMB !!!??

FCM

l<512

ILC

l<100

WFM

l<512

ErFM

l<512

Image analysis for non-Gaussianity test cross power spectrum

Pixel by pixel

WMAP KP masks cross power spectrum

Asymmetry of the CMB power cross power spectrum

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

NEP

SEP

Global anisotropy

of the Universe.

NEP

WHY ?

SEP

Gaussian Random Fields cross power spectrum

Strict 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 2p (by Central Limit Theorem)

transformed Planck cross power spectrum

Planck satellite and transformed Planck have the same power spectrum (same|dk|), they have different “faces” due to different phases:

It is phase Fk that keep Max’s face, not amplitude |dk| !!

Planck satellite

Max Planck

|dk| exp(iFk)

|dk|

exp(iFk)

|dk| exp(iFk)

FT-1[ ]

Asymmetry of the WMAP phases cross power spectrum

Asymmetry of the WMAP phases cross power spectrum

ILC

TOH

WTOH

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

M-1,M correlation

through - L direction

NO Evidence of Primordial Magnetic Field !

Naselsky, Verkhodanov, Novikov,Olesen,Chiang,ApJ,2004

Non-Gaussianity of the WMAP. cross power spectrum

WHY ?

NON-GAUSSIANITY cross power spectrum

Primordial

(Inflation ?)

Foregrounds + systematic

Df= DF + f *DF*DF

NEW

PHYSICS

S= G + NG

Summary 2003-2005 cross power spectrum

1.Residues of the foregrounds separation

Chiang ,Naselsky, Verkhodanov and Way,ApJ.Lett2003;

Naselsky , Doroshkevich and Verkhodanov,ApJ.Lett,2003;

Naselsky , Doroshkevich and Verkhodanov,MNRAS,2004;

Park, MNRAS,2004;

Eriksen, D.Novikov, Lille,Gorski, ApJ,2004 ;

Naselsky, Verkhodanov, Novikov,Olesen,Chiang,ApJ,2004,…

2. Systematic effects

Hansen, Vittorio,ApJ.Lett.2004 (+)

Vielva et al,MNRAS, 2004 (-)

3. Primordial

Bershadskii, Skrinevasan, Phys.Lett.,2003;2004 (magnetic field)

Vielva et al,MNRAS, 2004

Hansen, Bandy, Gorski,MNRAS,2004

Wandelt ,ApJ.Lett,2004

Non-Gaussianity is not a dog!” cross power spectrumYa.B.Zel’dovich

Sorry!

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