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Collaborators within DK- Planck community

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

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  1. 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)

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

  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 Gaussian or non-Gaussian Gaussian only !

  7. Cosmology before WMAP

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

  9. 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

  10. 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

  11. 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

  12. 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

  13. Reionization 300 Mpc 3Mpc

  14. WMAP ? PLANCK, 2007

  15. 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

  16. WMAP map: Gaussian by WMAP science team with 95% CL ! ? |f |<100 Df = DF + f *DF*DF

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

  18. The definition of Gaussianity

  19. 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

  20. FOREGROUNS + instrumental noise+ systematic effects

  21. 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

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

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

  24. WMAP KP masks

  25. Asymmetry of the CMB power

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

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

  28. NON-CMB L<100 L<512 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 2p (by Central Limit Theorem)

  31. 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[ ]

  32. Asymmetry of the WMAP phases

  33. Foreground-cleaned map m Foreground-cleaned map ℓ

  34. 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

  35. Non-Gaussianity of the WMAP. WHY ?

  36. NON-GAUSSIANITY Primordial (Inflation ?) Foregrounds + systematic Df= DF + f *DF*DF NEW PHYSICS S= G + NG

  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

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

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