WMAP 
FiveYear Wilkinson Microwave Anisotropy Probe (WMAP) Observations:

WMAP Fiveyear Paper Figures, J. Dunkley, et al.  
Individual figures are provided for use in talks. Proper display of PNG transparency in PowerPoint requires saving files to your computer before Inserting them. Please acknowledge the WMAP Science Team when using these images. 

Fig. 1 This figure compares the lowl TT power spectrum computed with two different techniques. At each l value, we plot the maximum likelihood value (tic mark), the region where the likelihood is greater than 50% of the peak value (thick line) and the region where the likelihood is greater than 95% of the peak value (thin line). The black lines (left side of each pair) are estimated by Gibbs sampling using the ILC map smoothed with a 5 degree Gaussian beam (at HEALPix N_{side} = 32). The light blue line (right side of the pair) is estimated with a pixelbased likelihood code with N_{side} = 16. The slight differences between the points are primarily due to differences in resolution. At each multipole, the likelihood is sampled by fxing the other C_{l} values at a fiducial spectrum (red). 
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Fig. 2 The temperature angular power spectrum corresponding to the WMAPonly bestfit ΛCDM model. The grey dots are the unbinned data; the black data points are binned data with 1σ error bars including both noise and cosmic variance computed for the bestfit model. 
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Fig. 3 Constraints on ΛCDM parameters from the fiveyear WMAP data. The twodimensional 68% and 95% marginalized limits are shown in blue. They are consistent with the threeyear constraints (grey). Tighter limits on the amplitude of matter fluctuations, σ_{8}, and the cold dark matter density Ω_{c}h^{2}, arise from a better measurement of the third temperature (TT) acoustic peak. The improved measurement of the EE spectrum provides a 5σ detection of the optical depth to reionization, Τ , which is now almost uncorrelated with the spectral index n_{s}. 
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Fig. 4 Constraints from the fiveyear WMAP data on ΛCDM parameters (blue), showing marginalized onedimensional distributions and twodimensional 68% and 95% limits. Parameters are consistent with the threeyear limits (grey) from Spergel et al. (2007), and are now better constrained. 
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Fig. 5 Left: marginalized probability distribution for z_{reion} in the standard model with instantaneous reionization. Sudden reionization at z = 6 is ruled out at 3.5s, suggesting that reionization was a gradual process. Right: in a model with two steps of reionization (with ionization fraction x_{e} at redshift z_{r}, followed by full ionization at z = 7), the WMAP data are consistent with an extended reionization process. 
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Fig. 6 Effect of foreground treatment and likelihood details on ΛCDM parameters. Left: The number of bands used in the template cleaning (denoted `T'), affects the precision to which τ is determined, with the standard KaQV compared to QV and KaQVW, but has little effect on other cosmological parameters. Using maps cleaned by Gibbs sampling (KKaQV (G)) also gives consistent results. Right: Lowering the residual point source contribution (`lower ptsrc') and removing the marginalization over an SZ contribution (`No SZ') affects parameters by < 0.4σ. Using a larger mask (`80% mask') has a greater effect, increasing Ω_{b}h^{2} by 0.5σ, but is consistent with the effects of noise. 
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Fig. 7 Bestfit temperature angular power spectrum from WMAP alone (red), which is consistent with data from recent smallscale CMB experiments: ACBAR, CBI, VSA, and BOOMERANG. 
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Fig. 8 Baryon Acoustic Oscillations expected for the bestfit ΛCDM model (red lines), compared to BAO in galaxy power spectra calculated from (left) combined SDSS and 2dFGRS main galaxies, and (right) SDSS LRG galaxies, by Percival et al. (2007a). The observed and model power spectra have been divided by P(k)_{smooth}, a smooth cubic spline fit described in Percival et al. (2007a). 
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Fig. 9 Red line shows the luminosityâ€“distance relationship predicted for the bestfit WMAPonlymodel (the right column in Table 2). The points show binned supernova observations from the Union compilation (Kowalski et al. 2008), including highredshift SNIa from Hubble Space Telescope (HST; Riess et al. 2007), ESSENCE (Miknaitis et al. 2007), and SNLS (Astier et al. 2006). The plot shows the deviation of the luminosity distances from the empty universe model. 
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Fig. 10 Twodimensional marginalized constraints (68% and 95% confidence levels) on inflationary parameters r, the tensortoscalar ratio, and n_{s}, the spectral index of fluctuations, defined at k_{0} = 0.002/Mpc. Onedimensional 95% upper limits on r are given in the legend. Left: the fiveyear WMAP data place stronger limits on r (shown in blue) than threeyear data (gray). This excludes some inflationary models including λφ^{4} monomial inflaton models with r ~ 0.27, ns ~ 0.95 for 60 efolds of inflation. Right: for models with a possible running spectral index, r is now more tightly constrained due to measurements of the third acoustic peak. Note: the twodimensional 95% limits correspond to Δ(2 ln L) ~ 6, so the curves intersect the r = 0 line at the ~ 2.5s limits of the marginalized ns distribution. 
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Fig. 11 Twodimensional marginalized limits for the spectral index, n_{s}, defined at k_{0} = 0.002/Mpc, and the running of the index dn_{s}/dln k (marked n_{run}). Models with no tensor contribution, and with a tensor contribution marginalized over, are shown. In both cases the models are consistent with a powerlaw spectral index, with dn_{s}/dln k = 0, as expected from the simplest in inflationary models. 
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Fig. 12 Marginalized twodimensional limits (68% and 95%) on the amplitude of possible CDM entropy (or isocurvature) fluctuations. The onedimensional 95% upper limits are given in the legend. Left: Anticorrelated fluctuations are tightly constrained, placing limits on curvaton models. Right: Uncorrelated fluctuations, corresponding to axion models for dark matter, add less power to the CMB spectrum than the anticorrelated case, for a given α. In both cases the amplitude is correlated with the spectral index of curvature fluctuations n_{s}, which compensates for the large scale power added by the CDM entropy fluctuations. 
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Fig. 13 Evidence for a nonzero effective number of neutrino species, N_{eff}. Left: The marginalized probability distribution gives N_{eff} > 2.3 (95% CL) from WMAP alone. The bestfit ΛCDM model with N_{eff} = 0 is a poorer fit to the data than N_{eff} = 3, with ΔX^{2} = 8.2. Right: Joint twodimensional distribution for N_{eff} and the CDM density, Ω_{c}h^{2}, with fiveyear limits in blue, compared to threeyear limits in grey. The degeneracy valley of constant z_{eq} is shown dashed, indicating that the CMB is now sensitive to the effect of neutrino anisotropic stress, which breaks the degeneracy. 
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Fig. 14 Comparison of the CMB angular power spectrum for the bestfit ΛCDM models with the standard N_{eff} = 3.04 neutrino species (red), and with N_{eff} = 0 species (blue). Bottom: The fractional difference between the two spectra when N_{eff} is increased from 0 to 3.04. The N_{eff} = 0 model has a lower Ω_{m}h^{2} in order to fit the third peak, and a lower spectral index, n_{s}, compared to the N_{eff} = 3.04 model. 
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Fig. 15 Limits on the sum of neutrino masses with the WMAP fiveyear data. Left: The marginalized onedimensional limit from WMAP alone is Σm_{v} < 1.3 eV (95% CL). This is raised by <10% with marginalization over a running spectral index, tensor fluctuations, or a dark energy equation of state w. Right: The neutrino mass is anticorrelated with σ_{8}, the amplitude of matter fluctuations. 
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Fig. 16 Left: The points show the set of nonflat models consistent with the WMAP data, colored by the Hubble constant values. The value of 2 lnL for all points shown is within 16 of the bestfit value. WMAP measures the acoustic peak scale to high accuracy, but does not constrain the curvature, Ω_{k}, by itself. However, the highly curved models have a low Hubble constant, inconsistent with observation. Right: Constraints on the dark energy equation of state, w, and the dark energy density, Ω_{Λ}, from WMAP alone. With a Hubble constant H_{0} < 100, weak limits can be placed on w in a flat universe, shown by the blue contours, but the dark energy density and equation of state are unconstrained (with the 95% confidence level shaded grey) if the assumption of flatness is relaxed. Limits are significantly improved when WMAP is combined with additional data (Komatsu et al. 2009). 
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Fig. 17 The angular power spectra of signal and noise components in the smoothed ILC map used for Gibbs sampling the lowl temperature spectrum. Uncorrelated noise, at 2 μK per pixel (red), is added to the smoothed ILC map to speed up the sampling, and then is assumed to be the only noise present. This assumption is inaccurate at low l, as it ignores the true noise (blue), but the error is negligible since it is significantly lower than cosmic variance (green). 
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Fig. 18 The level of variation in the lowell TT Gibbs likelihood that arises from different input parameters. The spectrum estimated from the standard input (black) is compared to results obtained using a different white noise realization (blue), using a larger mask (KQ80,red), and degrading to N_{side} = 16 (green) rather then 32. The likelihood does fluctuate with these changes, but has a negligible effect on cosmological parameters. The values shown at each multipole correspond to maximum likelihood values obtained by fixing the spectrum of other multipoles at fiducial values. The error bars show where the likelihood is at 50% and 5% of its peak value. 
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