WMAP 
NineYear Wilkinson Microwave Anisotropy Probe (WMAP) Observations:

WMAP Nineyear Paper Figures, Hinshaw, et al.  
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Fig.1 A compilation of the CMB data used in the nineyear WMAP analysis. The WMAP data are shown in black, the extended CMB data set  denoted 'eCMB' throughout  includes SPT data in blue (Keisler et al. 2011), and ACT data in orange, (Das et al. 2011b). We also incorporate constraints from CMB lensing published by the SPT and ACT groups (not shown). The ΛCDM model fit to the WMAP data alone (shown in grey) successfully predicts the higherresolution data. 
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Fig.2 Two estimates of the WMAP nineyear power spectrum along with the bestfit model spectra obtained from each; black  the C^{1}weighted spectrum and best fit model; red  the same for the MASTER spectrum and model. The two spectrum estimates differ by up to 5% in the vicinity of l ~ 50 which mostly affects the determination of the spectral index, n_{s}, as shown in Table 3. We adopt the C^{1}weighted spectrum throughout the remainder of this paper. 
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Fig.3 68% and 95% CL regions for the ΛCDM parameters n_{s}, 10^{9}Δ^{2}_{R}, and Ω_{b}h^{2}. There is a modest degeneracy between these three parameters in the sixparameter ΛCDM model, when fit to the nineyear WMAP data. The contours are derived from fits to the C^{1}weighted power spectrum, while the plus signs indicate the maximum likelihood point for the fit to the MASTER power spectrum. As shown in Figure 2, the two model produce nearly identical spectra. 
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Fig.4 Measurements of the scalar spectral index with CMB and BAO data. Left to right  contours of (D_{V} (0.57)/r_{s},n_{s}), (H_{0},n_{s}), (Ω_{c}h^{2},n_{s}). Black contours show constraints using WMAP nineyear data alone; blue contours include SPT and ACT data (WMAP+eCMB); red contours add the BAO prior(WMAP+eCMB+BAO). The BAO prior provides an independent measurement of the lowredshift distance, D_{v}(z)/r_{s}, which maps to constraints on Ω_{c}h^{2} and H_{0}. When combined with CMB data, the joint constraints require a tilt in the primordial spectral index (n_{s}< 1) at the 5σ level. 
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Fig.5 Measurements of Ω_{c}h^{2} and H_{0} from CMB data only (blue contours, WMAP+eCMB), from CMB and BAO data (green contours, WMAP+eCMB+BAO), and from CMB and H_{0} data (red contours, WMAP+eCMB+H_{0}). The two nonCMB priors push the constraints towards opposite ends of the range allowed by the CMB alone, but they are not inconsistent. 
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Fig.6 The nineyear WMAP data (in black) are shown with the 1σ locus of sixparameter ΛCDM models allowed by the nineyear WMAP data. The error band is derived from the Markov Chain of sixparameter model fits to the WMAP data alone. The blue curve indicates the mean of the ΛCDM model fit to the WMAP+eCMB data combination. At highl this curve sits about 1σ below the model fit to WMAP data alone. The marginalized parameter constraints that define these models are given in the WMAP and WMAP+eCMB columns of Table 4. 
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Fig.7 Twodimensional marginalized constraints (68% and 95% CL) on the primordial tilt, n_{s}, and the tensortoscalar ratio, r, derived with the nineyear WMAP in conjunction with: eCMB (green) and eCMB+BAO+H_{0} (red). The symbols and lines show predictions from singlefield inflation models whose potential is given by V (Φ) ∝ Φ^{α} (Linde 1983), with α = 4 (solid), α = 2 (longdashed), and α = 1 (shortdashed; McAllister et al. 2010). Also shown are those from the first inflation model, which is based on an R^{2} term in the gravitational Lagrangian (dotted; Starobinsky 1980). Starobinsky's model gives n_{s} = 12/N and r = 12/N^{2} where N is the number of efolds between the end of inflation and the epoch at which the scale k = 0.002 Mpc^{1} left the horizon during inflation. These predictions are the same as those of inflation models with a ξΦ^{2} R term in the gravitational Lagrangian with a λΦ^{4} potential (Komatsu & Futamase 1999). See Appendix A for details. 
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Fig.8 An illustration of four effects in the CMB anisotropy that can compensate for a change in the total radiation density, ρ_{r}, parameterized here by an effective number of neutrino species, N_{eff} . The filled circles with errors show the nineyear WMAP data (in black), the ACT data (in green, Das et al. 2011), and the SPT data (in violet, Keisler et al. 2011). The dashed lines show the bestfit model with N_{eff} = 3.046, while the solid lines show models with N_{eff} = 7 with selected adjustments applied. (The other parameters in the dashed model are Ω_{b}h^{2} = 0.02270, Ω_{c}h^{2} = 0.1107, H_{0} = 71.38 km/s/Mpc, n_{s} = 0.969, Δ^{2}R = 2.384 × 10^{9}, and τ = 0.0856.) Topleft: the laxis for the N_{eff} = 7 model has been scaled so that both models have the same angular diameter distance, d_{A}, to the surface of last scattering. Topright: the cold dark matter density, Ω_{c}h^{2}, has been adjusted in the N_{eff} = 7 model so that both models have the same redshift of matterradiation equality, z_{eq}. Bottomleft: the amplitude of the N_{eff} = 7 model has been rescaled to counteract the suppression of power that arises when the neutrino's anisotropic stress alters the metric perturbation. Bottomright: the helium abundance, Y_{P} , in the N_{eff} = 7 model has been adjusted so that both models have the same diffusion damping scale. 
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Fig.9 Joint, marginalized constraints (68% and 95% CL) on the primordial helium abundance, Y_{He}, and the energy density of "extra radiation species," parameterized as an effective number of neutrino species, N_{eff} . These constraints are derived from the nineyear WMAP+eCMB data (black), and from WMAP+eCMB+BAO+H0 data (red). The green curve shows the predicted dependence of Y_{He} on N_{eff} from Big Bang Nucleosynthesis; the dashed lines indicate the standard model: N_{eff} = 3.046, Y_{He} = 0.248. 
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Fig.10 The joint, marginalized constraint on w_{0} and w_{a}, assuming a flat universe. A cosmological constant (w_{0} = 1, w_{a} = 0) is at the boundary of the 68% CL region allowed by theWMAP+eCMB+BAO+H_{0}+SNe data, indicating that the current data are consistent with a nonevolving dark energy density. The shaded region is excluded by a hard prior, w_{a} < 0.2  1.1w_{0}, in our fits. 
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Fig.11 A compilation of the (Ω_{m}, σ_{8}) constraints from large scale structure observations, discussed in §5, compared to the constraints obtained from CMB, BAO, and H_{0} data. The various large scale structure probes do not separately constrain the two parameters, and have somewhat different degeneracy slopes among them, but these independent measurements are quite consistent. The following 1σ regions are plotted: (a) σ_{8}Ω^{0.5}_{m} = 0.465 ± 0.026 from Tinker et al. (2012); (b) σ_{8}(Ω_{m}/0.325)^{0.501} = 0.828 ± 0.049 from Zu et al. (2012); (c) σ_{8}(Ω_{m}/0.25)^{0.47} = 0.813 ± 0.032 from Vikhlinin et al. (2009b); (d) σ_{8}(Ω_{m}/0.25)^{0.3} = 0.785 ± 0.037 from Benson et al. (2011); (e) σ_{8}(Ω_{m}/0.3)^{0.67} = 0.70^{+0.11}_{0.14} from Semboloni et al. (2011); (f ) σ_{8}Ω^{0.7}_{m} = 0.252^{+0.032}_{0.052} from Lin et al. (2012); (g) WMAP only; (h) WMAP+eCMB+BAO+H_{0}; (i) ellipse whose major and minor axes are given by Ωm = 0.259±0.045 and σ_{8} = 0.748±0.035 from Hudson & Turnbull (2012). 
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Fig.12 Coadded maps of temperature, T, and polarization, Qr, smoothed to a common resolution of 0.5°, and stacked by the location of temperature extrema. (The polarization maps were not smoothed for the analysis, however.) Topleft: the average temperature hot spot. Topright: the rotated polarization map, Qr, stacked around temperature hot spots. Bottomleft: the average temperature cold spot. Bottomright: the rotated polarization map, Qr, stacked around temperature cold spots. The polarization images are colorcoded so that the red (Qr > 0) shows the radial polarization pattern, while blue (Qr < 0) shows the tangential polarization pattern. The lines indicate polarization direction. These images are a striking illustration of BAO in the early plasma, and phase coherence in their initial conditions. 
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