1. Collaborators within DK-Planck community 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

2. Non-Gaussianity of the CMB sky P.Naselsky NBI, the PLANCK scientist Why the issue of Non-Gaussianity is important for development of cosmology ?

3. “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!!

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

5. Picture of the Quantum fluctuations from Inflation in radio waves

6. Definition of the power spectra Definition of the power spectra Gaussian or non-Gaussian Gaussian only !

7. Cosmology before WMAP

8. The temperature anisotropy and temperature polarization cross power spectrum Precision cosmology !!!

9. BOOMERANG, MAXIMA-1,CBI,ARCHEOPS,VSA,DASI, BIMA +……. SN1a, 2dF,He,D… CMB Ω h =0.02 ! b 2 WMAP +……. SN1a, 2dF,He, D WHY NOT FOR US ? Cosmologyof Cosmology of the XX century the XX century

10. Important question is WHY? Dark matter density Dark energy density ≈1/3 1/ π ? (D=3)/(D=10) ? What about Extra dimensions ? Topology ? Baryonic matter density Dark matter density ? Baryosynthesis? Cosmologyof the XXI century Cosmology of the XXI century

11. Development of Cosmology and High energy physics Dark energy Dark matter Baryonic matter } Φ(x, t)=Ψ(x, t)* exp [iΛ(x, t)] exp [iΛ(x, t)] S.Bonometto et al,2004,2005

12. Non linear theory of dark energy-dark matter coupling 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

13. 300 Mpc 3Mpc Reionization

14. WMAP PLANCK,2007

15. Two news from the WMAP data analysis team ) Komatsu et al, 2003 (WMAP team ) 2. The CMB signal is non- Gaussian non- Gaussian

16. WMAP map: Gaussian by WMAP science team with 95% CL  f   f 

17. , Non-Gaussianity is not a dog!” Ya.B.Zel’dovich Ya.B.Zel’dovich ΔΦΔΦ f*ΔΦΔΦ

18. The definition of Gaussianity

19. Methods of detection of Non-Gaussianity in the WMAP sky Image domainMultipoles 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 is Non-Gaussian

20. FOREGROUNS + instrumental noise+ systematic effects

21. CMB maps derived from the WMAP data ILC l<100 FCM l<512 WFM l<512 ErFM l<512 NOT FOR INVESTIGA- INVESTIGA- TION OF THE CMB !!!?? CMB !!!??

22. Image analysis for non-Gaussianity test Pixel by pixel

23. Foregrounds ? FCM-ErFCM ILC-ErFCM ILC-WFM V band l=400

24. WMAP KP masks

25. Asymmetry of the CMB power

26. *South-north asymmetry of the COBE and the WMAP signals. Global anisotropy of the Universe. NEP SEP WHY ?

27. Non-CMB tools Q-W V-W FCM WFCM FCM-WFCM MV

28. L<512 NON-CMB L<100 L<30

29. Alignment of the low multipoles Schwarz et al,2004

30. 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  (by Central Limit Theorem)

31. 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(i  k ) |k||k|exp(i  k )

32. Asymmetry of the WMAP phases

33. Foreground-cleaned map ℓ m

34. Asymmetry of the WMAP phases L-1,L+1 correlation through m- direction M-1,M correlation through - L direction ILC WTOH TOH NO Evidence of Primordial Magnetic Field ! Naselsky, Verkhodanov, Novikov,Olesen,Chiang,ApJ,2004

35. Non-Gaussianity of the WMAP. WHY ?

36. Primordial (Inflation ?) Foregrounds + systematic NON-GAUSSIANITY NEW PHYSICS S= G + NG  f 

37. 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

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