1. Results from Three- Year WMAP Observations Eiichiro Komatsu (UT Austin) TeV II Particle Astrophysics August 29, 2006

2. Why Care About WMAP? WMAP observes CMB. This is a conference about “TeV” particle astrophysics. Why care about CMB? –The present-day temperature of CMB is 2.725K, or 2.35 meV. –The temperature at decoupling (where the most of CMB is coming from) was ~3000K, or 0.26 eV. –The temperature at matter-radiation equality was ~9000K, or 0.8 eV. CMB is a nuisance for many particle astrophysicists: it attenuates cosmic-ray particles traveling through the universe. (GZK) Why am I here?

3. What Can CMB Offer? Baryon-to-photon ratio in the universe –Sound speed and inertia of baryon-photon fluid Matter-to-radiation ratio in the universe –Dark matter abundance –“ Radiation ” may include photons, neutrinos as well as any other relativistic components. Angular diameter distance to decoupling surface –Peak position in l space ~ (Sound horizon)/(Angular Diameter Distance) Time dependence of gravitational potential –Integrated Sachs-Wolfe Effect, Dark energy Primordial power spectrum (Scalar+Tensor) –Constraints on inflationary models Optical depth –Cosmic reionization

4. Full Sky Microwave Map COBE/FIRAS : T=2.725 K Uniform, “ Fossil ” Light from the Big Bang Cosmic Microwave Background Radiation

5. COBE/FIRAS, 1990 Perfect blackbody = Thermal equilibrium = Big Bang

6. COBE/DMR, 1992 Gravity is STRONGER in cold spots:  T/T~ 

7. The Wilkinson Microwave Anisotropy Probe A microwave satellite working at L2 Five frequency bands –K (22GHz), Ka (33GHz), Q (41GHz), V (61GHz), W (94GHz) The Key Feature: Differential Measurement –The technique inherited from COBE –10 “ Differencing Assemblies ” (DAs) –K1, Ka1, Q1, Q2, V1, V2, W1, W2, W3, & W4, each consisting of two radiometers that are sensitive to orthogonal linear polarization modes. Temperature anisotropy is measured by single difference. Polarization anisotropy is measured by double difference.

8. K band (22GHz)

9. Ka Band (33GHz)

10. Q Band (41GHz)

11. V Band (61GHz)

12. W Band (94GHz)

13. The Angular Power Spectrum CMB temperature anisotropy is very close to Gaussian; thus, its spherical harmonic transform, a lm, is also Gaussian. Since a lm is Gaussian, the power spectrum: completely specifies statistical properties of CMB.

14. WMAP 3-yr Power Spectrum

15. Physics of CMB Anisotropy SOLVE GENERAL RELATIVISTIC BOLTZMANN EQUATIONS TO THE FIRST ORDER IN PERTURBATIONSSOLVE GENERAL RELATIVISTIC BOLTZMANN EQUATIONS TO THE FIRST ORDER IN PERTURBATIONS

16. Use temperature fluctuations,  =  T/T, instead of f: Expand the Boltzmann equation to the first order in perturbations: where describes the Sachs-Wolfe effect : purely GR fluctuations.

17. For metric perturbations in the form of: the Sachs-Wolfe terms are given by where  is the directional cosine of photon propagations. Newtonian potential Curvature perturbations 1.The 1st term = gravitational redshift 2.The 2nd term = integrated Sachs-Wolfe effect h 00 /2  h ij /2 (higher T)

18. When coupling is strong, photons and baryons move together and behave as a perfect fluid. When coupling becomes less strong, the photon-baryon fluid acquires shear viscosity. So, the problem can be formulated as “ hydrodynamics ”. (c.f. The Sachs-Wolfe effect was pure GR.) Small-scale Anisotropy (<2 deg) Collision term describing coupling between photons and baryons via electron scattering.

19. Boltzmann Equation to Hydrodynamics Monopole: Energy density Dipole: Velocity Quadrupole: Stress Multipole expansion Energy density, Velocity, Stress

20. Photon Transport Equations f 2 =9/10 (no polarization), 3/4 (with polarization)  A = -h 00 /2,  H = h ii /2  C =Thomson scattering optical depth CONTINUITY EULER Photon-baryon coupling

21. Baryon Transport Cold Dark Matter

22. The Strong Coupling Regime SOUND WAVE!

23. The Wave Form Tells Us Cosmological Parameters Higher baryon density  Lower sound speed  Compress more  Higher peaks at compression phase (even peaks)

24. What CMB Measures Amplitude of temperature fluctuations at a given scale, l  4008002004010010 Multipole moment l~  Small scalesLarge scales Ang.Diam. Distance Baryon-to- photon Ratio Mat-to- Radiatio n Ratio ISW

25. CMB to Parameters

26. Measuring Matter-Radiation Ratio where  is the directional cosine of photon propagations. 1.The 1st term = gravitational redshift 2.The 2nd term = integrated Sachs-Wolfe effect h 00 /2  h ij /2 (higher T) During the radiation dominated epoch, even CDM fluctuations cannot grow (the expansion of the Universe is too fast); thus, dark matter potential gets shallower and shallower as the Universe expands --> potential decay --> ISW --> Boost C l.

27. Matter-Radiation Ratio More extra radiation component means that the equality happens later. Since gravitational potential decays during the radiation era (free-fall time scale is longer than the expansion time scale during the radiation era), ISW effect increases anisotropy at around the Horizon size at the equality.

28. How Many (Effective) Neutrinos?

29. So, It ’ s Been Three Years Since The First Data Release. What Is New Now?

30. POLARIZATION DATA!!

31. K Band (23 GHz) Dominated by synchrotron; Note that polarization direction is perpendicular to the magnetic field lines.

32. Ka Band (33 GHz) Synchrotron decreases as -3.2 from K to Ka band.

33. Q Band (41 GHz) We still see significant polarized synchrotron in Q.

34. V Band (61 GHz) The polarized foreground emission is also smallest in V band. We can also see that noise is larger on the ecliptic plane.

35. W Band (94 GHz) While synchrotron is the smallest in W, polarized dust (hard to see by eyes) may contaminate in W band more than in V band.

36. Polarized Light Filtered Polarized Light Un-filtered

37. Jargon: E-mode and B-mode Polarization is a rank-2 tensor field. One can decompose it into a divergence- like “E-mode” and a vorticity-like “B-mode”. E-modeB-mode Seljak & Zaldarriaga (1997); Kamionkowski, Kosowsky, Stebbins (1997)

38. Physics of CMB Polarization Thomson scattering generates polarization, if … –Temperature quadrupole exists around an electron –Where does quadrupole come from? Quadrupole is generated by shear viscosity of photon-baryon fluid, which is generated by velocity gradient. electron isotropic anisotropic no net polarization net polarization

39. Boltzmann Equation Temperature anisotropy, , can be generated by gravitational effect (noted as “SW” = Sachs-Wolfe) Linear polarization (Q & U) is generated only by scattering (noted as “C” = Compton scattering). Circular polarization (V) would not be generated. (Next slide.)

40. Primordial Gravity Waves Gravity waves create quadrupolar temperature anisotropy -> Polarization Directly generate polarization without kV. Most importantly, GW creates B mode.

41. Power Spectrum Scalar T Tensor T Scalar E Tensor E Tensor B

42. Polarization From Reionization CMB was emitted at z~1088. Some fraction of CMB was re-scattered in a reionized universe. The reionization redshift of ~11 would correspond to 365 million years after the Big-Bang. z=1088,  ～ 1 z ～ 11,  ～ 0.1 First-star formation z=0 IONIZED REIONIZED NEUTRAL

43. Measuring Optical Depth Since polarization is generated by scattering, the amplitude is given by the number of scattering, or optical depth of Thomson scattering: which is related to the electron column number density as Ne =

44. Polarization from Reioniazation “ Reionization Bump ”

45. Outside P06 –EE (solid) –BB (dashed) Black lines –Theory EE tau=0.09 –Theory BB r=0.3 Frequency = Geometric mean of two frequencies used to compute C l Masking Is Not Enough: Foreground Must Be Cleaned Rough fit to BB FG in 60GHz

46. Clean FG Only two-parameter fit! Dramatic improvement in chi-squared. The cleaned Q and V maps have the reduced chi-squared of ~1.02 per DOF=4534 (outside P06)

47. BB consistent with zero after FG removal. 3-sigma detection of EE. The “Gold” multipoles: l=3,4,5,6.

48. Parameter Determination: First Year vs Three Years The simplest LCDM model fits the data very well. –A power-law primordial power spectrum –Three relativistic neutrino species –Flat universe with cosmological constant The maximum likelihood values very consistent –Matter density and sigma8 went down slightly

49. What Should WMAP Say About Flatness? Flatness, or very low Hubble ’ s constant? If H=30km/s/Mpc, a closed universe with Omega=1.3 w/o cosmological constant still fits the WMAP data.

50. Constraints on GW Our ability to constrain the amplitude of gravity waves is still coming mostly from the temperature spectrum. –r<0.55 (95%) The B-mode spectrum adds very little. WMAP would have to integrate for at least 15 years to detect the B-mode spectrum from inflation.

51. What Should WMAP Say About Inflation Models? Hint for ns<1 Zero GW The 1-d marginalized constraint from WMAP alone is ns=0.95+-0.02. GW>0 The 2-d joint constraint still allows for ns=1 (HZ).

52. What Should WMAP Say About Dark Energy? Not much! The CMB data alone cannot constrain w very well. Combining the large-scale structure data or supernova data breaks degeneracy between w and matter density.

53. What Should WMAP Say About Neutrino Properties? 3.04)

54. Understanding of –Noise, –Systematics, –Foreground, and Analysis techniques have significantly improved from the first- year release. A simple LCDM model fits both the temperature and polarization data very well. CMB offers constraints on: Neutrino properties: the number of species and mass Dark matter abundance Dark matter abundance and properties Inflationary models (flatness and spectral index) Reionization of the universe We are now working on the 5-year data… Summary