1. Gary Hinshaw NASA/GSFC From Quantum to Cosmos, Airlie Center VA, July 8 2008 5-year Results from WMAP with a Glimpse Ahead

2. WMAP Mission WMAP’S PURPOSE – To make a detailed full-sky map of the CMB radiation anisotropy (temperature and polarization) to constrain the cosmology of our universe.

3. W = Wilkinson WMAP Science Team

4. WMAP’s Differential Receivers* 10 “Differencing Assemblies” 4 @ 94 GHz W-band 2 @ 61 GHz V-band 2 @ 41 GHz Q-band 1 @ 33 GHz Ka-band 1 @ 23 GHz K-band *based on HEMT design of M. Pospieszalski

5. WMAP Launch June 30, 2001 at 3:47 EDT Delta II Model 7425-10 Delta Launch Number 286 Star-48 third stage motor Cape Canaveral Air Force Station Pad SLC-17B

6. WMAP at L2

7. Taken with ESO 2.2 m telescope, La Silla Chile, for GAIA optical tracking test. 3 images (R,G.B) taken a few minutes apart, V=19.4.

8. WMAP Sky Coverage Not to scale: Earth — L2 distance is 1% of Sun — Earth Distance Earth Sun MAP at L 2 1 Day 3 Months 6 Months - full sky coverage 129 sec. (0.464rpm) Spin 22.5° half-angle 1 hour precession cone A-side line of site B-side line of site MAP990159

9. 5-year Temperature Maps

10. 5-year Polarization Maps

11. 5-year Absolute Calibration New dipole fitting technique yields absolute gain accuracy of <0.2% (difference between red and black curves).

12. 5-year Beam Calibration Major effort to model beam response down to -44 dB allows us to model PSF response with factor of ~2 improvement in accuracy. (Hill et al.) Jupiter data Physical model Residual Jupiter data Physical model Residual A side B side

13. 3-year Power Spectrum - TT

14. 5-year Power Spectrum - TT

15. Important Dates Inflation – initial conditions: A, r, n s Dark ages → first stars – polarization: τ Plasma epoch – matter, radiation content: Ω b, Ω c Large scale structure – dark energy: Ω Λ, σ 8

16. 5-year ΛCDM Parameters Blue curves/contours – 5-year data Grey curves/contours – 3-year data Biggest improvements in: Optical depth, τ Amplitude of fluctuations @ 8 Mpc, σ 8 Matter densities, Ω b h 2, Ω c h 2

17. TE EE Was reionization a complex process? Low-l TE and EE polarization power spectra can distinguish between different ionization histories. Plots show mean TE, EE spectra for range of reionization histories. Reionization - I

18. Reionization - II Improved polarization data improves measurement of optical depth and/or reionization redshift. Also begin to probe 2 nd reionization parameter. The bulk of the reionization had to occur at z>6, thus it had to be an extended process.

19. Cosmic Neutrino Background Evidence for the cosmic neutrino background, “would provide the most dramatic possible confirmation of the standard model of the early universe” The First Three Minutes Steven Weinberg 1977 On seeing evidence for the cosmic neutrino background

20. New limits on gravitational wave amplitude, r<0.2. Information still largely comes from shape of TT spectrum. Testing Inflation - I

21. “Named” inflation models are currently being put to the test. Many of the models predict an observable gravitational wave background (via the CMB B-mode polarization). Testing Inflation - II

22. Future WMAP Operations WMAP is nearing 7 years at L2 and has been approved for 2 final years of operation. What important questions will more WMAP data help address? Reionization - was reionization an extended process? Was the universe partially reionized at z = 20 or 30? Dark Energy - upcoming dark energy experiments will be limited by WMAP cosmological parameter uncertainties. Additional WMAP data will improve these uncertainties. Physics of Inflation - primordial gravity waves, primordial non-Gaussianity, deviations from scale invariance. Also: polarized synchrotron data, radio source & planet data, calibration source for ground/balloon-based experiments

23. 4/24/2008WMAP 2008 Senior Review23 Output counts per unit of input temperature difference changes with time due to changes in spacecraft temperature and amplifier properties. Multiple years of data help to separate these effects and improve uncertainty in the gain model. Change in instrument offset vs. time. Additional years of data improve our knowledge of the sources of offset: thermal emission, gain variation, etc. Detailed Understanding of Instrument

24. TT 5-Yr

25. TT 9-Yr

26. TE 5-Yr

27. TE 9-Yr

28. EE

29. Dark Energy WMAP5 and the Cluster Mass Function K. Rines, A. Diaferio & P. Natarajan arXiv:0803.1843 Growth Function Combined LSS and CMB measurements probe Dark Energy. Improvements in cluster counts (Chandra, ROSAT, SDSS, DES, Pan-STARRS, etc.) and weak lensing surveys will demand better measurements of  8 and  m to constrain w(z). The predicted number of massive clusters (alternatively, the SZ power spectrum) scales as  8 7 ! Acoustic scale WMAP measures the sound horizon at z=1090. This acoustic scale is the fundamental calibration for on-going and planned baryon acoustic oscillation measurements. l A = 302.08 ± 0.84 (5 yr) → ± 0.64 (9 yr) (30% improvement)

30. Closing in on  8 and  m 2006 Chandra cluster counts: Vikhlinin et al. 2008+

31. Inflation Have we detected deviations from scale-invariance? ~2.5 σ Is there a running spectral index? Probably not. Is there primordial non-Gaussianity? Not yet… What is the amplitude of tensor modes (gravitational waves)? r<0.2

32. Testing Inflation

33. Future CMB From Space Planck Spacecraft is integrated, launch is imminent! See next talk. CMBPol High sensitivity polarization to probe gravity waves from Inflation.

34. Inflation and Gravity Waves - I Inflation predicts two forms of fluctuations: –Scalar modes (density perturbations) with slope n s : generate CMB anisotropy and lead to structure formation –Tensor modes (gravity waves) with slope n t : generate CMB anisotropy but do not contribute to structure formation Gravity wave amplitude, r, proportional to energy scale of inflation: Both types of fluctuations contribute to CMB temperature anisotropy:

35. Inflation and Gravity Waves – II Both types of fluctuations contribute to CMB polarization anisotropy: –Scalar modes produce only “E-mode” polarization patterns, by symmetry –Tensor modes produce both “E-mode” and “B-mode” polarization patterns (see below) The observation of B-mode polarization uniquely separates scalar and tensor modes from inflation and measures the energy scale of inflation. Only known probe of physics at E ~ 10 16 GeV… 12 orders of magnitude higher than planned accelerators. E – scalar+tensor B – tensor only

36. Sensitivity & Foreground Estimates Blue band - Galactic foreground estimate from WMAP3, frequency dependent Green line - Lensing (EE→BB), frequency independent Red lines - Gravity wave signal(s) Grey shaded band - 1-sigma sensitivity for 1000-channel system with 1-yr integration, 1°FWHM resolution r=0.01 r=0.3

37. Candidate CMBPol Concept Multiple copies of basic polarimeter module, scaled in frequency, packaged in focal plane, co-aligned along s/c symmetry axis.

38. 4/24/2008WMAP 2008 Senior Review38

39. Monodromy in the CMB: Gravity Waves and String Inflation Eva Silverstein and Alexander Westphal http://arxiv.org/abs/0803.3085v2 Large-field inflation (hence gravitational waves) from string theory compactified on twisted tori.