WMAP 
SevenYear Wilkinson Microwave Anisotropy Probe (WMAP) Observations:

WMAP Sevenyear 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.1 Coordinate system for Stokes Q and U. We use Galactic coordinates with north up and east left. In this example, Q_{r} is always negative, and U_{r} is always zero. When Q_{r} > 0 and U_{r} = 0, the polarization pattern is radial. 
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Fig.2 Temperaturepolarization cross correlation with various smoothing functions. (Left) The TE power spectrum with no smoothing is shown in the black solid line. For the other curves, the temperature is always smoothed with a 0.5° (FWHM) Gaussian, whereas the polarization is smoothed with either the same Gaussian (black dashed), Qband beam (blue solid), Vband beam (purple solid), or Wband beam (red dashed). (Right) The corresponding spatial temperatureQ_{r} correlation functions. The vertical dotted lines indicate (from left to right): the acoustic scale, 2×the acoustic scale, and 2×the horizon size, all evaluated at the decoupling epoch. 
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Fig.3 Predicted temperature peakpolarization cross correlation, as measured by the stacked profile of the transformed Stokes Q_{r}, computed from equation (11) for various values of the threshold peak heights. The temperature is always smoothed with a 0.5° (FWHM) Gaussian, whereas the polarization is smoothed with either the same Gaussian (black dashed), Qband beam (blue solid), Vband beam (purple solid), or Wband beam (red dashed). (Top left) All temperature hot spots are stacked. (Top right) Spots greater than 1σ are stacked. (Bottom left) Spots greater than 2σ are stacked. (Bottom right) Spots greater than 3σ are stacked. The light gray lines show the average of the measurements from noiseless simulations with a Gaussian smoothing of 0.5° FWHM. The agreement is excellent. 
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Fig.4 Predicted temperature peaktemperature correlation, as measured by the stacked temperature profile, computed from equation (13) for various values of the threshold peak heights. The choices of the smoothing functions and the threshold peak heights are the same as in Figure 3. 
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Fig.5 Stacked images of temperature and polarization data around temperature cold spots. Each panel shows a 5° × 5° region with north up and east left. Both the temperature and polarization data have been smoothed to a common resolution of 0.5°. (Top) Simulated images with no instrumental noise. From left to right: the stacked temperature, Stokes Q, Stokes U, and transformed Stokes Q_{r} (see equation (1)) overlaid with the polarization directions. (Middle) WMAP 7year V+W data. In the observed map of Q_{r}, the compression phase at 1.2° and the reversal phase at 0.6° are clearly visible. (Bottom) Null tests. From left to right: the stacked Q_{r} from the sum map and from the difference map (VW)/2, the stacked U_{r} from the sum map and from the difference map. The latter three maps are all consistent with noise. Note that U_{r}, which probes the TB correlation (see equation (12)), is expected to vanish in a parityconserving universe. 
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Fig.6 Same as Figure 5 but for temperature hot spots. 
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Fig.7 The WMAP 7year temperature power spectrum (Larson et al. 2010), along with the temperature power spectra from the ACBAR (Reichardt et al. 2009) and QUaD (Brown et al. 2009) experiments. We show the ACBAR and QUaD data only at l ≥ 690, where the errors in the WMAP power spectrum are dominated by noise. We do not use the power spectrum at l > 2000 because of a potential contribution from the SZ effect and point sources. The solid line shows the bestfitting 6parameter flat ΛCDM model to the WMAP data alone (see the 3rd column of Table 1 for the maximum likelihood parameters). 
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Fig.8 Limits on the tensortoscalar ratio, r, from the polarization data (BB, EE and TE) alone. All the other cosmological parameters, including the optical depth, are fixed at the 5year bestfit ΛCDM model (Dunkley et al. 2009). The vertical axis shows 2 ln(L/L_{max}), where L is the likelihood and L_{max} is the maximum value. This quantity may be interpreted as the standard Χ^{2}, as the likelihood is approximately a Gaussian near the maximum; thus, 2 ln(L/L_{max}) = 4 corresponds to the 95.4% CL limit. The solid, dashed and dotdashed lines show the likelihood as a function of r from the BBonly, BB+EE, and BB+EE+TE data. (Left) The 7year polarization data. We find r < 2.1, 1.6, and 0.93 (95.4% CL) from the BBonly, BB+EE, and BB+EE+TE data, respectively. (Right) The 5year polarization data. We find r < 4.7, 2.7, and 1.6 (95.4% CL) from the BBonly, BB+EE, and BB+EE+TE data, respectively. 
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Fig.9 Constraint on the effective number of neutrino species, N_{eff}. (Left) Joint twodimensional marginalized distribution (68% and 95% CL), showing how a better determination of H_{0} improves a limit on Ω_{m}h^{2}. (Middle) A correlation between N_{eff} and Ω_{m}h^{2}. The dashed line shows the line of correlation given by equation (58). A better determination of H_{0} improves a limit on Ω_{m}h^{2} which, in turn, improves a limit on N_{eff}. (Right) Onedimensional marginalized distribution of N_{eff} from WMAPonly and WMAP+BAO+H_{0}. The 68% interval from WMAP+BAO+H_{0}, N_{eff} = 4.34^{+0.86}_{0.88}, is consistent with the standard value, 3.04, which is shown by the vertical line. 
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Fig.10 Primordial helium abundance and the temperature power spectrum. The data points are the same as those in Figure 7. The lower (pink) solid line (which is the same as the solid line in Figure 7) shows the power spectrum with the nominal helium abundance, Y_{p} = 0.24, while the upper (blue) solid line shows that with a tiny helium abundance, Y_{p} = 0.01. The larger the helium abundance is, the smaller the number density of electrons during recombination becomes, which enhances the Silk damping of the power spectrum on small angular scales, l ≥500. 
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Fig.11 Constraint on the primordial helium abundance, Y_{p}. (Left) Joint twodimensional marginalized distribution (68% and 95% CL), showing that Y_{p} and Ω_{b}h^{2} are essentially uncorrelated. (Middle) A slight correlation exists between Y_{p} and n_{s}: an enhanced Silk damping produced by a larger Y_{p} can be partially canceled by a larger n_{s}. (Right) Onedimensional marginalized distribution of Y_{p} from WMAPonly and WMAP+ACBAR+QUaD. The 68% interval from WMAP+ACBAR+QUaD, Y_{p} = 0.326 ± 0.075 is consistent with the nominal value, 0.24, which is shown by the vertical line. 
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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}. The contours show the 68% and 95% CL from WMAP+BAO+H_{0} (red), WMAP+BAO+H_{0}+D_{Δ}_{t} (black), and WMAP+BAO+SN (purple). 
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Fig.13 Joint twodimensional marginalized constraint on the linear evolution model of dark energy equation of state, w(a) = w_{0} + w_{a}(1  a). The contours show the 68% and 95% CL from WMAP+H_{0}+SN (red), WMAP+BAO+H_{0}+SN (blue), and WMAP+BAO+H_{0}+D_{Δ}_{t}+SN (black), for a flat universe. 
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Fig.14 Angular radial profile of the SZ effect toward the Coma cluster, in units of the RayleighJeans (RJ) temperature (µK). While the V (green) and Wband (blue) measurements are contaminated by the CMB fluctuations around Coma, our optimal estimator can separate the SZ effect and CMB when the V and Wband measurements are combined (red). The solid line shows the bestfitting spherical β model with the core radius of θ_{c} = 10.5 arcmin and β = 0.75. The bestfitting central temperature decrement (fit to a β model) is T_{SZ,RJ}(0) = 377±105 µK. Note that 10 arcmin corresponds to the physical distance of 0.195 h^{1} Mpc at the location of Coma. The radius within which the mean overdensity is 500 times the critical density of the universe, r_{500}, corresponds to about 50 arcmin. 
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Fig.15 Angular radial profiles of the SZ effect toward nearby massive clusters (with M_{500} ≥ 4×10^{14} h^{1} M_{SUN} and z ≤ 0.09), in units of the RayleighJeans (RJ) temperature (μK). The V and Wband data are combined optimally to separate the CMB and the SZ effect. All of these clusters have θ_{500} ≥ 14′, i.e., resolved by the WMAP beam. The masses, M_{500} are MY given in the 6th column of Table 2 in Vikhlinin et al. (2009a), times h_{vikhlinin} = 0.72 used by them, except for Coma. For Coma, we estimate M500 using the masstemperature relation given in Vikhlinin et al. (2009a) with the temperature of 8.45 keV (Wik et al. 2009). The dashed lines show the expected SZ effect from the Xray data on the individual clusters, whereas the solid lines show the prediction from the average pressure profile found by Arnaud et al. (2009). Note that Coma is not included in the sample of Vikhlinin et al. (2009a), and thus the Xray data are not shown. We find that Arnaud et al.′s profiles overpredict the gas pressure (hence the SZ effect) of noncooling flow clusters. Note that all coolingflow clusters are "relaxed," and all noncoolingflow clusters are "nonrelaxed" (i.e., morphologically disturbed), according to the criterion of Vikhlinin et al. (2009a). 
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Fig.16 Average temperature profile of the SZ effect from the stacking analysis, in units of the RayleighJeans (RJ) temperature (µK), at θ = 7, 35, 63, and 91 arcmin. The V and Wband data are combined using the optimal estimator. (Top) The SZ effect measured from the locations of clusters of galaxies. The results with three different maximum redshifts, z_{max} = 0.1 (blue; left), 0.2 (green; middle), and 0.45 (red; right), are shown. The error bars include noise due to the CMB fluctuation, and thus are correlated (see equation (82) for the correlation matrix). (Middle) A null test showing profiles measured from random locations on the sky (for z_{max} = 0.2; the number of random locations is the same as the number of clusters used in the top panel). Three random realizations are shown. Our method does not produce biased results. (Bottom) The measured profile (z_{max} = 0.2) is compared with the model profiles derived from Xray observations (Arnaud et al. 2009) and theoretically calculated from hydrostatic equilibrium (Komatsu & Seljak 2001) with two different concentration parameters. Note that the model profiles are calculated also for z_{max} = 0.2 but have not been multiplied by the bestfitting normalization factors given in Table 12. 
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Fig.17 Gas pressure profiles of clusters of galaxies, P_{gas}(r), at z = 0.1, and the projected profiles of the SZ effect, ΔT_{SZ}(θ) (RayleighJeans temperature in µK). (Top Left) The gas pressure profiles. The upper and bottom set of curves show M_{500} = 3×1014 and 3 × 10^{13}h^{1} M_{sun}, respectively. The horizontal axis shows radii scaled by the corresponding r_{500} = 0.78 and 0.36 h^{1} Mpc, respectively. The solid lines show P_{gas}(r) = P_{e}(r)/0.518 derived from Xray observations (Arnaud et al. 2009), while the dotted and dashed lines show P_{gas}(r) predicted from hydrostatic equilibrium (Komatsu & Seljak 2001) with NFW concentration parameters of Seljak (2000) and Duffy et al. (2008), respectively. (Top Right) The projected SZ profiles computed from the corresponding curves in the top left panel and equation (87). The horizontal axis shows angular radii scaled by θ_{500} = r_{500}/D_{A}, which is 10 and 4.7 arcmin for M_{500} = 3 × 1014 and 3 × 1013 h^{1} M_{sun}, respectively. (Bottom Left) Same as the top left panel, but the dotted and dashed lines show Pgas(r) predicted from “Cooling+Star Formation” and “Nonradiative” simulation runs by Nagai et al. (2007). (Bottom Right) Same as the top right panel, but the dotted and dashed lines are computed from the corresponding curves in the bottom left panel and equation (87). 
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Fig.18 Gas mass fraction as a function of M_{500}. The thick horizontal line shows the cosmic mean baryon fraction, Ω_{b}/Ω_{m} = 0.167. The solid line shows the gas mass fraction, f_{gas} = M_{gas,500}/M_{500}, derived from Xray observations (Vikhlinin et al. 2009a), while the dotted and dashed lines show fgas predicted from hydrostatic equilibrium (Komatsu & Seljak 2001) with NFW concentration parameters of Seljak (2000) and Duffy et al. (2008), respectively. 
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Fig.19 Distribution of M_{500} estimated from clusters in the catalog using the measured X_{ray} luminosities in 0.12.4 keV band, L_{X}, and equations (89) and (C2). The light blue, dark blue, and pink histograms show z_{max} = 0.45, 0.2, and 0.1, respectively. 
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Fig.20 Twodimensional joint marginalized constraint (68% and 95% CL) on the primordial tilt, n_{s}, and the tensortoscalar ratio, r, derived from the data combination of WMAP+BAO+H_{0}. The symbols show the predictions from “chaotic” inflation models whose potential is given by V (Φ) ∝ Φ^{α} (Linde 1983), with α = 4 (solid) and α = 2 (dashed) for singlefield models, and α = 2 for multiaxion field models with β = 1/2 (dotted; Easther & McAllister 2006). 
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