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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)

slide2

Why the issue of

Non-Gaussianity

is important for

development

of cosmology ?

Non-Gaussianity of the CMB sky

P.Naselsky

NBI, the PLANCK scientist

slide3

“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!!

slide4

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

slide5

Picture of the

Quantum fluctuations from

Inflation in radio waves

definition of the power spectra
Definition of the power spectra

Gaussian or

non-Gaussian

Gaussian only !

the temperature anisotropy and temperature polarization cross power spectrum
The temperature anisotropy and temperature polarization cross power spectrum

Precision

cosmology !!!

slide9

WMAP +……. 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

slide10

Cosmologyof 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

slide11

Dark energy

}

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

slide12

Non linear theory of dark energy-dark matter

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

slide13

Reionization

300 Mpc

3Mpc

slide14

WMAP

?

PLANCK,

2007

slide15

Two news from the WMAP data analysis

  • The CMB signal is
  • Gaussian !

Komatsu et al, 2003 (WMAP team )

2. The CMB signal is

non- Gaussian

slide17

Non-Gaussianity is not a dog!”

Ya.B.Zel’dovich

,

f*ΔΦΔΦ

slide19

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 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

slide20

FOREGROUNS +

instrumental noise+

systematic effects

slide21

CMB maps derived from the WMAP data

NOT FOR

INVESTIGA-

TION OF THE

CMB !!!??

FCM

l<512

ILC

l<100

WFM

l<512

ErFM

l<512

slide23

Foregrounds ?

ILC-ErFCM

FCM-ErFCM

V band l=400

ILC-WFM

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

NEP

SEP

Global anisotropy

of the Universe.

NEP

WHY ?

SEP

slide27

Non-CMB tools

Q-W

FCM

WFCM

V-W

FCM-WFCM

MV

slide28

NON-CMB

L<100

L<512

L<30

gaussian random fields
Gaussian Random Fields

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)

slide31

transformed Planck

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[ ]

slide33

Foreground-cleaned map

m

Foreground-cleaned map

asymmetry of the wmap phases1
Asymmetry of the WMAP phases

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

slide36

NON-GAUSSIANITY

Primordial

(Inflation ?)

Foregrounds + systematic

Df= DF + f *DF*DF

NEW

PHYSICS

S= G + NG

summary 2003 2005
Summary 2003-2005

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

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