Three-Year WMAP Observations: Method and Results

1. Three-Year WMAP Observations: Method and Results Eiichiro Komatsu Department of Astronomy HEP Seminar, April 27, 2006

2. David Wilkinson (1935~2002) • Science Team Meeting, July, 2002

3. 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.

4. WMAP Spacecraft upper omni antenna back to back line of sight Gregorian optics, 1.4 x 1.6 m primaries 60K passive thermal radiator focal plane assembly feed horns secondary 90K reflectors thermally isolated instrument cylinder 300K warm spacecraft with: medium gain antennae - instrument electronics - attitude control/propulsion - command/data handling deployed solar array w/ web shielding - battery and power control MAP990422

5. WMAP Focal Plane • 10 DAs (K, Ka, Q1, Q2, V1, V2, W1-W4) • Beams measured by observing Jupiter.

6. WMAP Goes To L2 0.010 • June 30, 2001 • Launch • Phasing loop • July 30, 2001 • Lunar Swingby • October 1, 2001 • Arrive at L2 • October 2002 • 1st year data • February 11, 2003 • 1st data release • October 2003 • 2nd year data • October 2004 • 3rd year data • March 16, 2006 • 2nd data release 0.005 Earth Y (AU) L2 0.000 -0.005 -0.010 1.000 1.005 1.010 X (AU)

7. K band (22GHz)

8. Ka Band (33GHz)

9. Q Band (41GHz)

10. V Band (61GHz)

11. W Band (94GHz)

12. Intensity Mask

13. The Angular Power Spectrum • CMB temperature anisotropy is very close to Gaussian; thus, its spherical harmonic transform, alm, is also Gaussian. • Since alm 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 PERTURBATIONS

16. Use temperature fluctuations, Q=DT/T, instead off: 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: Newtonian potential Curvature perturbations the Sachs-Wolfe terms are given by wheregis the directional cosine of photon propagations. • The 1st term = gravitational redshift • The 2nd term = integrated Sachs-Wolfe effect h00/2 (higher T) Dhij/2

18. Small-scale Anisotropy (<2 deg) • 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 shearviscosity. • So, the problem can be formulated as “hydrodynamics”. (c.f. The Sachs-Wolfe effect was pure GR.) Collision term describing coupling between photons and baryons via electron scattering.

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

20. CONTINUITY EULER Photon-baryon coupling Photon Transport Equations f2=9/10 (no polarization), 3/4 (with polarization) FA = -h00/2, FH = hii/2 tC=Thomson scattering optical depth

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. Weighing Dark Matter wheregis the directional cosine of photon propagations. • The 1st term = gravitational redshift • The 2nd term = integrated Sachs-Wolfe effect h00/2 (higher T) Dhij/2 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 Cl.

25. Weighing Dark Matter • Smaller dark matter density • More time for potential to decay • Higher first peak

26. Measuring Geometry Sound cross. length • W=1 • W<1

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

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

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

30. 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.

31. 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.

32. Polarization Mask fsky=0.743

33. Seljak & Zaldarriaga (1997); Kamionkowski, Kosowsky, Stebbins (1997) 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-mode B-mode

34. Polarized Light Un-filtered Polarized Light Filtered

35. 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 no net polarization anisotropic net polarization

36. Boltzmann Equation • Temperature anisotropy, Q, 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.)

37. Sources of Polarization • Linear polarization (Q and U) will be generated from 1/10 of temperature quadrupole. • Circular polarization (V) will NOT be generated. No source term, if V was initially zero.

38. Monopole Dipole Photon Transport Equation Quadrupole f2=3/4 FA = -h00/2, FH = hii/2 tC=Thomson scattering optical depth

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

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

41. 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. IONIZED z=1088, t～1 NEUTRAL First-star formation z～11, t～0.1 REIONIZED z=0

42. 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

43. Polarization from Reioniazation “Reionization Bump”

44. Masking Is Not Enough: Foreground Must Be Cleaned • 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 Cl Rough fit to BB FG in 60GHz

45. 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)

46. 3-sigma detection of EE. The “Gold” multipoles: l=3,4,5,6. BB consistent with zero after FG removal.

47. 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

48. 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.

49. 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).

50. 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.