WMAP 
FiveYear Wilkinson Microwave Anisotropy Probe (WMAP) Observations:

WMAP Fiveyear Paper Figures, E. Komatsu, 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. Image Credit: NASA / WMAP Science Team 

Fig. 01 Constraint on the primordial tilt, n_{s} (ξ 3.1.2). No running index or gravitational waves are included in the analysis. (Left) Onedimensional marginalized constraint on n_{s} from the WMAPonly analysis. (Middle) Twodimensional joint marginalized constraint (68% and 95% CL), showing a strong degeneracy between n_{s} and Ω_{b}h^{2}. (Right) A mild degeneracy with τ . None of these degeneracies improve signifcantly by including BAO or SN data, as these data sets are not sensitive to Ω_{b}h^{2} or τ however, the situation changes when the gravitational wave contribution is included (see Fig. 3). 
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Fig. 02 How the WMAP temperature and polarization data constrain the tensortoscalar ratio, r. (Left) The contours show 68% and 95% CL. The gray region is derived from the lowl polarization data (TE/EE/BB at l ≤ 23) only, the red region from the lowl polarization plus the highl TE data at l ≤ 450, and the blue region from the lowl polarization, the highl TE, and the lowl temperature data at l ≤ 32. (Right) The gray curves show (r, τ ) = (10, 0.050), the red curves (r, τ ) = (1.2, 0.075), and the blue curves (r, τ ) = (0.20, 0.080), which are combinations of r and τ that give the upper edge of the 68% CL contours shown on the left panel. The vertical lines indicate the maximum multipoles below which the data are used for each color. The data points with 68% CL errors are the WMAP 5year measurements (Nolta et al. 2008). (Note that the BB power spectrum at l ~ 130 is consistent with zero within 95% CL.) 
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Fig. 03 Constraint on the tensortoscalar ratio, r, at k = 0.002 Mpc^{1} (ξ 3.2.4). No running index is assumed. See Fig. 4 for r with the running index. In all panels we show the WMAPonly results in blue and WMAP+BAO+SN in red. (Left) Onedimensional marginalized distribution of r, showing the WMAPonly limit, r < 0.43 (95% CL), and WMAP+BAO+SN, r < 0.20 (95% CL). (Middle) Joint twodimensional marginalized distribution (68% and 95% CL), showing a strong degeneracy between n_{s} and r. (Right) Degeneracy between n_{s} and Ω_{m}h^{2}. The BAO and SN data help to break this degeneracy which, in turn, reduces the degeneracy between r and n_{s}, resulting in a factor of 2.2 better limit on r. 
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Fig. 04 Constraint on the tensortoscalar ratio, r, the tilt, n_{s}, and the running index, dn_{s}/d ln k, when all of them are allowed to vary (ξ 3.2.4). In all panels we show the WMAPonly results in blue and WMAP+BAO+SN in red. (Left) Joint twodimensional marginalized distribution of n_{s}, and r at k = 0.002 Mpc^{1} (68% and 95% CL). (Middle) n_{s} and dn_{s}/d ln k. (Right) dn_{s}/d ln k and r. We find no evidence for the running index. While the inclusion of the running index weakens our constraint on n_{s}, and r, the data do not support any need for treating the running index as a free parameter. 
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Fig. 05 Constraint on three representative inflation models whose potential is positively curved, V″ > 0 (ξ 3.3). The contours show the 68% and 95% CL derived from WMAP+BAO+SN. (Top) The monomial, chaotictype potential, V(φ) ∝ φ^{∝} (Linde 1983), with α = 4 (solid) and α = 2 (dashed) for singlefield models, and α = 2 for multiaxion field models with β = 1/2 (Easther & McAllister 2006) (dotted). The symbols show the predictions from each of these models with the number of efolds of inflation equal to 50 and 60. The λφ^{4} potential is excluded convincingly. (Middle) The exponential potential, V (Φ) ∝ exp[(Φ/M_{pl})√2/p], which leads to a powerlaw inflation, a(t) ∝ t^{p} (Abbott & Wise 1984; Lucchin & Matarrese 1985). All models but p ~ 120 are outside of the 68% region. For multifield models these limits can be translated into the number of fields as P → np_{i}, where p_{i} is the pparameter of each field (Liddle et al. 1998), the data favour n ~ 120/p_{i} fields, where p_{i} is the pparameter of each field. (Bottom) The hybridtype potential, V(φ) =V_{0} + (1/2)m^{2}φ^{2} = V_{0}(1 + φ^{2}), where φ ≡ mφ/(2V_{0})^{1/2} (Linde 1994). The models with φ < 2/3 drive inflation by the vacuum energy term, V_{0}, and are disfavoured at more than 95% CL, while those with φ > 1 drive inflation by the quadratic term, and are similar to the chaotic type (the left panel with α = 2). The transition regime, 2/3 < φ < 1 are outside of the 68% region, but still within the 95% region. 
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Fig. 06 Joint twodimensional marginalized constraint on the vacuum energy density, Ω_{Λ}, and the spatial curvature parameter, Ω_{k} (ξ 3.4.3). The contours show the 68% and 95% CL. (Left) The WMAPonly constraint (light blue) compared with WMAP+BAO+SN (purple). Note that we have a prior on Ω_{Λ}, Ω_{Λ} > 0. This figure shows how powerful the extra distance information is for constraining Ω_{k}. (Middle) A blowup of the region within the dashed lines in the left panel, showing WMAPonly (light blue), WMAP+HST (gray), WMAP+SN (dark blue), and WMAP+BAO (red). The BAO provides the most stringent constraint on Ω_{k}. (Right) Onedimensional marginalized constraint on Ω_{k} from WMAP+HST, WMAP+SN, and WMAP+BAO. We find the best limit, 0.0181 < Ω_{k} < 0.0071 (95% CL), from WMAP+BAO+SN, which is essentially the same as WMAP+BAO. See Fig. 12 for the constraints on Ω_{k} when dark energy is dynamical, i.e., w ≠1, with timeindependent w. 
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Fig. 07 Minkowski functionals from the WMAP 5year data, measured from the templatecleaned V+W map at Nside = 128 (28' pixels) outside of the KQ75 mask. From the top to bottom panels, we show the Euler characteristics (also known as the genus), the contour length, and the cumulative surface area, as a function of the threshold (the number of σ's of hot and cold spots), ν≡ ΔT/σ_{0}. (Left) The data (symbols) are fully consistent with the mean and dispersion of Gaussian realizations that include CMB and noise. The gray bands show the 68% intervals of Gaussian realizations. (Right) The residuals between the WMAP data and the mean of the Gaussian realizations. 
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Fig. 08 Constraint on the axion entropy perturbation fraction, α_{0} (ξ 3.6.3). In all panels we show the WMAPonly results in blue and WMAP+BAO+SN in red. (Left) Onedimensional marginalized constraint on α_{0}, showing WMAPonly and WMAP+BAO+SN. (Middle) Joint twodimensional marginalized constraint (68% and 95% CL), showing the degeneracy between α_{0} and n_{s} for WMAPonly and WMAP+BAO+SN. (Right) Degeneracy between n_{s} and Ω_{m}h^{2}. The BAO and SN data help to break this degeneracy which, in turn, reduces degeneracy between α_{0} and n_{s}, resulting in a factor of 2.4 better limit on α_{0}. 
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Fig. 09 Constraint on the curvaton entropy perturbation fraction, α_{1} (ξ 3.6.4). In all panels we show the WMAPonly results in blue and WMAP+BAO+SN in red. (Left) Onedimensional marginalized constraint on α_{1}, showing WMAPonly and WMAP+BAO+SN. (Middle) Joint twodimensional marginalized constraint (68% and 95% CL), showing the degeneracy between α_{1} and n_{s} for WMAPonly and WMAP+BAO+SN. (Right) Degeneracy between n_{s} and Ω_{m}h^{2}. The BAO and SN data help to break this degeneracy which, in turn, reduces degeneracy between α_{1} and n_{s}, resulting in a factor of 3 better limit on α_{1}. These properties are similar to those of the axion dark matter presented in Fig. 8. 
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Fig. 10 Constraint on the polarization rotation angle, Δα, due to a parityviolating interaction that rotates the polarization angle of CMB (ξ 4.3). We have used the polarization spectra (TE/TB/EE/BB/EB at l ≤ 23, and TE/TB at l ≥ 24), and did not use the TT power spectrum. (Left) Onedimensional marginalized constraint on Δα in units of degrees. The dark blue, light blue, and red curves show the limits from the lowl (2 ≤ l ≤ 23), highl (24 ≤ l ≤ 450), and combined (2 ≤ l ≤ 450) analysis of the polarization data, respectively. (Right) Joint twodimensional marginalized constraint on τ and Δα (68% and 95% CL). The bigger contours are from the lowl analysis, while the smaller ones are from the combined analysis. The vertical dotted line shows the bestfitting optical depth in the absence of parity violation (τ = 0.086), whereas the horizontal dotted line shows Δα = 0 to guide eyes. 
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Fig. 11 Constraint on the timeindependent (constant) dark energy equation of state, w, and the presentday dark energy density, Ω_{Λ}, assuming a flat universe, Ω_{k} = 0 (ξ 5.2). Note that we have imposed a prior on w, w > 2.5. (Left) Joint twodimensional marginalized distribution of w and Ω_{k}. The contours show the 68% and 95% CL. The WMAPonly constraint (light blue) is compared with WMAP+HST (gray), WMAP+BAO (red), WMAP+SN (dark blue), and WMAP+BAO+SN (purple). This figure shows how powerful a combination of the WMAP data and the current SN data is for constraining w. (Middle) Onedimensional marginalized constraint on w for a flat universe from WMAP+HST (gray), WMAP+BAO (red), and WMAP+SN (dark blue). The WMAP+BAO+SN result (not shown) is essentially the same as WMAP+SN. (Right) Onedimensional marginalized constraints on w for a flat universe from WMAP+HST (gray), WMAP+BAO (red), and WMAP+SN (dark blue). 
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Fig. 12 Joint twodimensional marginalized constraint on the timeindependent (constant) dark energy equation of state, w, and the curvature parameter, Ω_{k} (ξ 5.3). Note that we have imposed a prior on w, w > 2.5. The contours show the 68% and 95% CL. (Left) The WMAPonly constraint (light blue; 95% CL) compared with WMAP+BAO+SN (purple; 68% and 95% CL). This figure shows how powerful the extra distance information from BAO and SN is for constraining Ω_{k} and w simultaneously. (Middle) A blowup of the left panel, showing WMAP+HST (gray), WMAP+BAO (red), WMAP+SN (dark blue), and WMAP+BAO+SN (purple). This figure shows that we need both BAO and SN to constrain Ω_{k} and w simultaneously: WMAP+BAO fixes Ω_{k}, and WMAP+SN fixes w. (Right) The same as the middle panel, but with the BAO prior reweighted by a weaker BAO prior from the SDSS LRG sample (Eisenstein et al. 2005). The BAO data used in the other panels combine the SDSS main and LRG, as well as the 2dFGRS data (Percival et al. 2007). The constraints from these are similar, and thus our results are not sensitive to the exact form of the BAO data sets. 
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Fig. 13 Joint twodimensional marginalized constraint on the timeindependent (constant) dark energy equation of state, w, and the curvature parameter, Ω_{k}, derived solely from the WMAP distance priors (l_{A}, R, z_{*}) (see ξ 5.4.1), combined with either BAO (red) or SN (dark blue) or both (purple). The contours show the ΔX^{2} _{total} = 2.30 (68.3% CL) and ΔX^{2} _{total} = 6.17 (95.4% CL). The left (BAO data from Percival et al. (2007)) and right (BAO data from Eisenstein et al. (2005)) panels should be compared with the middle and right panels of Fig. 12, respectively, which have been derived from the full WMAP data combined with the same BAO and SN data. While the WMAP distance priors capture most of the information in this parameter space, the constraint is somewhat weaker than that from the full analysis. 
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Fig. 14 Constraint on models of timedependent dark energy equation of state, w(z) (Eq. [70]), derived from the WMAP distance priors (l_{A}, R, and z_{*}) combined with the BAO and SN distance data (ξ 5.4.2). There are three parameters: w_{0} is the value of w at the present epoch, w_{0} ≡ w(z = 0), w' is the first derivative of w with respect to z at z = 0, w' ≡ dw/dz_{z=0}, and z_{trans} is the transition redshift above which w(z) approaches to 1. Here, we assume flatness of the universe, Ω_{k} = 0. (Left) Joint twodimensional marginalized distribution of w_{0} and w' for z_{trans} = 10. The constraints are similar for the other values of z_{trans}. The contours show the ΔX^{2} total = 2.30 (68.3% CL) and ΔX^{2} total = 6.17 (95.4% CL). (Middle) Onedimensional marginalized distribution of w_{0} for z_{trans} = 0.5 (dotted), 2 (dashed), and 10 (solid). (Middle) Onedimensional marginalized distribution of w_{0} for z_{trans} = 0.5 (dotted), 2 (dashed), and 10 (solid). The constraints are similar for all ztrans. We do not find evidence for the evolution of dark energy. 
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Fig. 15 Constraint on the linear evolution model of dark energy equation of state, w(z) = w_{0} + w' z/(1 + z), derived from the WMAP distance priors (l_{A}, R, and z_{*}) combined with the BAO and SN distance data as well as the Big Bang Nucleosynthesis (BBN) prior (Eq. [71]). Here, we assume flatness of the universe, Ω_{k} = 0. (Left) Joint twodimensional marginalized distribution of w_{0} and w'. The contours show the ΔX^{2} _{total} = 2.30 (68.3% CL) and ΔX^{2} _{total} = 6.17 (95.4% CL). (Middle) Onedimensional marginalized distribution of w_{0}. (Middle) Onedimensional marginalized distribution of w'. We do not find evidence for the evolution of dark energy. Note that Linder (2003) defines w' as the derivative of w at z = 1, whereas we define it as the derivative at z = 0. They are related by w'_{linder} = 0.5w'_{WMAP}. 
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Fig. 16 Predictions for the presentday amplitude of matter fluctuations, σ_{8}, as a function of the (constant) dark energy equation of state parameter, w, derived from the full WMAP data (blue) as well as from WMAP+BAO+SN (red). The contours show the 68% and 95% CL. (Left) Flat universe, Ω_{k} = 0. (Right) Curved universe, Ω_{k}≠0. 
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Fig. 17 Constraint on the total mass of neutrinos, Σm_{ν} (ξ 6.1.3). In all panels we show the WMAPonly results in blue and WMAP+BAO+SN in red. (Left) Joint twodimensional marginalized distribution of H_{0} and Σm_{ν} (68% and 95% CL). The additional distance information from BAO helps reduce the degeneracy between H_{0} and Σm_{ν}. (Middle) The WMAP data, combined with the distances from BAO and SN, predict the presentday amplitude of matter fluctuations, σ_{8}, as a function of Σm_{ν} . An independent determination of σ_{8} will help determine Σm_{ν} tremendously. (Right) Joint twodimensional marginalized distribution of w and Σm_{ν}. No significant degeneracy is observed. Note that we have a prior on w, w > 2.5, and thus the WMAPonly lower limit on w in this panel cannot be trusted. 
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Fig. 18 Constraint on the effective number of neutrino species, N_{eff} (ξ 6.2.3). Note that we have imposed a prior on N_{eff}, 0 < N_{eff} < 10. In all panels we show the WMAPonly results in blue and WMAP+BAO+SN in red. (Left) Joint twodimensional marginalized distribution (68% and 95% CL), showing a strong degeneracy between Ω_{m} h^{2} and N_{eff}. This degeneracy line is given by the equality redshift, 1+z_{eq} = Ω_{m}/Ω_{r} =(4.050 x 10^{4} Ω_{m}h^{2}/(1+0.2271N_{eff}). The thick solid lines show the 68% and 95% limits calculated from the WMAPonly limit on z_{eq}: z_{eq} = 3141^{+154}_{157} (68%CL). The 95% CL contours do not follow the lines below N_{eff} ~ 1.5 but close there, which shows strong evidence for the cosmic neutrino background from its effects on the CMB power spectrum via the neutrino anisotropic stress. The BAO and SN provide an independent constraint on Ω_{m}h^{2}, which helps reduce the degeneracy between N_{eff} and Ω_{m}h^{2}. (Middle) When we transform the horizontal axis of the left panel to z_{eq}, we observe no degeneracy. (Right) Onedimensional marginalized distribution of N_{eff} from WMAPonly and WMAP+BAO+SN+HST. Note that a gradual decline of the likelihood toward N_{ eff} ≥∼ 6 for the WMAPonly constraint should not be trusted, as it is affected by the hard prior, N_{eff} < 10. The WMAP+BAO+SN+HST constraint is robust. This figure shows that the lower limit on N_{eff} is coming solely from the WMAP data. The 68% interval from WMAP+BAO+SN+HST, N_{eff} = 4.4 ± 1.5, is consistent with the standard value, 3.04 (vertical line). 
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Fig. 19 Four representative cosmological parameters that have improved significantly by adding the BAO and SN data. (See also Table 1.) The contours show the 68% and 95% CL. The WMAPonly constraint is shown in blue, while WMAP+BAO+SN in red. (Left) The distance information from BAO and SN provides a better determination of Ω_{m}h^{2}, which results in 40% better determination of σ_{8}. (Right) The BAO data, being the absolute distance indicator, provides a better determination of H_{0}, which results in a factor of 2 better determination of Ω_{Λ}, Ω_{b}, and Ω_{c}. 
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Fig C1 Evolution of dark energy for w_{0} = 1.1 and w' = 1, and various transition redshifts, z_{trans} = 0.5, 2, and 10, above which w(z) approaches to 1. (Top Left) Evolution of the dark energy to matter density ratio as a function of z. Note that the vertical axis has been multiplied by 10^{6}. (Top Right) Evolution of the dark energy density relative to the dark energy density at present. The dark energy density was nearly constant at high redshifts above z_{trans}; thus, these models can describe the "thawing models," (Caldwell & Linder 2005) in which dark energy was nearly constant at early times, and had become dynamical at lower redshifts. (Bottom Left) Evolution of the equation of state, w(z) = P_{de}(z)/ρ_{de}(z). By construction of the model, w(z) approaches to 1 beyond z_{trans}. (Bottom Right) Evolution of the effective equation of state, w_{eff}(z), which determines the evolution of dark energy density as ρ_{de}(z) = ρ_{de}(0)(1 + z)^{3[ 1+weff(z)]}. 
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Fig D1 The same as Fig. 15, but the systematic errors in the Type Ia supernova data are included. 
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