Recent results on measurements and interpretation of CMB fluctuations

1. Recent results on measurementsand interpretation of CMB fluctuations A. Doroshkevich Astro Space Center of the Physical Institute RAS Moscow, Russia

2. List of the problems • Observations of the CMB • Separation of the CMB and galactic foregrounds • Power spectrum of the CMB • Polarizations of the CMB • Standard cosmological model • Anomalies of the WMAP results • Extensions and limitations of the • cosmological models

3. OBSERVATIONS WMAP 23,30, 40, 60, 90 GHz, 1<l<950 ATACAMA 148,218, 277 GHz, 6m, 600<l<8000 BICEP 100, 150, 220 GHz, 21<l<335 QUaD 100, 150 GHz, 2.6m, 200<l<2000 SPT 95, 150, 220 GHz,2000<l<9500

4. WMAP observationsν= 22.8, 33.0, 40.7, 60.8, 93.5 GHzλ= 1.3, 0.9, 0.7, 0.5, 0.3 cmθ~20’, ΔT~3-5 10-6 K

5. Separation of the CMB and galactic foreground Incorrect problem (2 ↔ 3): ILC approach Observed signal S(θi) is superposition of the CMB signal C(θi)and Galactic foreground F(θi) • S1(θi)=C(θi)+F1(θi), S2(θi)=C(θi)+F2(θi), • For the homogeneous sample of pixels (ILC) • C(θi)=α S1(θi)+(1-α) S2(θi)=C+F2+α(F1–F2) • α=-<Q2Q12>/<Q122> • Q1 =S1-<S1>, Q2 =S2-<S2>, Q12 =Q1-Q2 • <Q1> =0, <Q2>=0, <Q12>=0

6. Decompositionof temperature – power spectrum here Φlm and alm are the phase and amplitude of fluctuations. Power spectrum of fluctuations is The shape of the power spectrum is well known for many cosmological models

7. 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[ ]

8. WMAP-7 power spectrum

9. WMAP-ACBAR – QUAD power spectrum

10. ATACAMA power spectrum

11. POLARIZATION • Compton scatter of CMB (E-mode) • 2<l<20 – reionization, (z~10) • l>20 – recombination, (z~1000) On the scalar modes l>2 (E-modes) • and vortex and tensor modes (B modes)

12. WMAP-7

13. Polarization around the temperature cold spot(simulation,observationV+Wand noiseV+/-W)

14. Polarization aroundthe temperature hot spot(simulations,observationsV+Wand noiseV+/-W)

15. BICEP-2010, (low l<300)

16. QUAD (l>300)

17. QUAD

18. Parameters of the cosmological model

20. Main results of the WMAP • 1. Complex reconstruction of the cosmological • model • Six parameters fit • In contrast with SN1 • Comparison with the Planck mission – • Tensor – scalar , r, ratio and • the redshift of reionization zreio • Multi parametric fits

21. Problems of this high precision separation: anomalies • 1. Quadrupole ΔT2=249μK2 • instead of the expected ΔT2=1250μK2 • 2. Axis of evil - common alignment of • quadrupole and octupole • 3. Asymmetry between north and south • hemispheres • 4. System of deep walls

23. Possible explanations • Small quadrupole and cold spots can be • explained with the anisotropic cosmology • The axis of evil and north – south asymmetry • can point out the unknown noise. • Bennett et al., 2011, ApJS,192,17B: • all anomalies are random effects • Doroshkevich, Verkhodanov, 2011, PhRvD, 83,043002: • The first three anomalies are caused by • bad separation between the CMB and foregrounds

24. Separation between the CMB and foreground - ILC approaches • The CMB map itself is interesting for purposes: • Homogeneity and isotropy of the Universe – • anisotropic cosmological models • Possible signatures of non-trivial topology • and mirror symmetry. • Correlations of the CMB with other emissions • Signatures of non Gaussianity of the CMB • Discussion in Delabrouille et al. arXiv:0807.0773 • Our corrections of the ILC approach: • It is unstable – discret instability

25. Correction of the power spectra

26. Bulk Flows KSZ - WMAP 263 – 48; (Kashlinsky & Atrio 2009) Galactic rotation (z<0.04) 52 – 68 (Longo 2011) CMB Quadrupole WMAP-7 283 – 65; 360 – 63; 15 – 26; ΔT22= 249μK2 CMB Quadrupole DV-11 285 – 9; 13 - 170; 60 – 77; ΔT22=1070μK2 Anisotropic cosmology(Perivolaropoulos arXiv:1104.0539)

27. Anisotropic cosmology (9 Bianchi models) • Anisotropy of cosmological expansion only • Anisotropy of the curvature of the Universe • Homogeneous magnetic field • Matter rotation • All four causes lead to quadrupole anisotropy • We can measure the combine effect only in a framework of anisotropic cosmological model • These effects are relatively small – • Demianski, Doroshkevich, 2007,PhRvD, 75, 123517

28. Small scale fluctuations - SZ effect KSZ as the standard candle

29. South Pole observations

30. The end The end

31. WMAP

32. BICEP

34. Parameters of the cosmological model

35. QUAD 100 & 150 GHz

36. WMAP Model 4ΔT22=249μK2 , ΔT22=1070μK2

38. WMAP-7

39. ILC separation for two channels • S1(θi)=C(θi)+F1(θi), S2(θi)=C(θi)+F2(θi), • For the homogeneous sample • C(θi)=α S1(θi)+(1-α) S2(θi), • α=-<Q2Q12>/<Q122> • Q1 =S1-<S1>, Q2 =S2-<S2>, Q12 =Q1-Q2 • <Q1> =0, <Q2>=0, <Q12>=0 • At the same timethe precise solution is • αf(<F2>-<F1>)= <F2>, αf=<F2>/(<F2>-<F1>)=α • What is the homogeneous sample??? >

40. TSZ – KSZ theory

41. SPT – SZ & DSFG

42. BULK FLOW of CLUSTERS • Method – KSZ from WMAP (l, b)D=263, 48

43. ACBAR

44. QUAD