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Collaborators within DK- Planck community. 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). Why the issue of

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Collaborators within dk planck community
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)


Why the issue of

Non-Gaussianity

is important for

development

of cosmology ?

Non-Gaussianity of the CMB sky

P.Naselsky

NBI, the PLANCK scientist


“BIG BANG”

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
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
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


Reionization cross power spectrum

300 Mpc

3Mpc


WMAP cross power spectrum

?

PLANCK,

2007


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

!

?

|f |<100

Df = DF + f *DF*DF


Non-Gaussianity is not a dog!” cross power spectrum

Ya.B.Zel’dovich

,

f*ΔΦΔΦ


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


FOREGROUNS + cross power spectrum

instrumental noise+

systematic effects


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


Foregrounds ? cross power spectrum

ILC-ErFCM

FCM-ErFCM

V band l=400

ILC-WFM


WMAP KP masks cross power spectrum


Asymmetry of the cmb power
Asymmetry of the CMB power cross power spectrum


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

NEP

SEP

Global anisotropy

of the Universe.

NEP

WHY ?

SEP


Non-CMB tools cross power spectrum

Q-W

FCM

WFCM

V-W

FCM-WFCM

MV


NON-CMB cross power spectrum

L<100

L<512

L<30


Alignment of the low multipoles cross power spectrum

Schwarz et al,2004

?


Gaussian random fields
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
Asymmetry of the WMAP phases cross power spectrum


Foreground-cleaned map cross power spectrum

m

Foreground-cleaned map


Asymmetry of the wmap phases1
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
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
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 ya b zel dovich
Non-Gaussianity is not a dog!” cross power spectrumYa.B.Zel’dovich

Sorry!


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