First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Interpretation of the TT and TE Angular Power Spectrum Peaks, L. Page, et al., 2003, ApJS, 148, 233, reprint / preprint (288 Kb) / individual figures / ADS / astro-ph

WMAP First-year Paper Figures, L. Page, 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 Binned WMAP data are shown as boxes, the maximum likelihood peak model from the peak fitting functions is shown as the solid line, and the uncertainties are shown as closed contours. The top panel shows the TT angular power spectrum. The bottom panel shows the TE angular cross-power spectrum. For each peak or trough, the contours from the MCMC chains are multiplied by a uniform prior and so they are equal to contours of the a posteriori likelihood of the data given the model. The contours are drawn at Δχ^{2} = 2.3 and 6.18 corresponding to 1σ and 2σ.

Fig.2 WMAP data in the Ω_{m}-h plane. The thick solid contours in black are at Δχ^{2} = - 2.3, -6.18 (1σ, 2σ) of the marginalized likelihood from the full analysis (Spergel et al. 2003). The filled region is the constraint from the position of the first peak, with ω_{b} = 0.023 fixed. In effect, it shows how Ω_{m} and h must be related to match the observed position of the first peak in a flat geometry or, equivalently, to match the measured values of θ_{A}. The darker inner region corresponds to 1σ, and the lighter outer region corresponds to 2σ. The dotted lines are isochrons separated by 1 Gyr. It is clear that the WMAP data pick out 13.6 Gyr for the age of the universe in the flat, w = -1 case. The dashed lines show the 1σ limits on ω_{m}. The light dashed line shows Ω_{m}h^{3.4} = constant.

Fig.3 Left: Parameter restrictions from H_{2}^{TT} in the ω_{b} - ns plane. The gray swath is the 1&sigma band corresponding to H_{2}^{TT} = 0.426 ± 0.015 with ω_{m} = 0.14. The swath is broadened if one includes the uncertainty in ω_{m}. The light gray swath is 2σ. The solid line in the middle of the swath is for ΔH_{2}^{TT} = Δω_{m} = 0. The contours are from the full analysis of just the WMAP data and are thus more restrictive. Right: The constraints in the ω_{b}-ω_{c} plane from the peak ratios in a flat geometry with n_{s} = 0.99. The darker shaded regions in each swath are the 1σ allowed range; the lighter shaded regions show the 2σ range. The horizontal swath is for H_{2}^{TT} = 0.426 ± 0.015, and the vertical one is for H_{3}^{TT} = 0.42 ± 0.08. The leftmost vertical line is for H_{2}^{TE} = 0.33 ± 0.10. The uncertainty band for H_{2}^{TE} is not shown as it is broader than the H_{3}^{TT} swath. The heavier central lines correspond to ΔH_{2}^{TT} = 0, ΔH_{3}^{TT} = 0, and ΔH_{2}^{TE} = 0, each with Δn_{s} = 0. As the mission progresses, all uncertainties will shrink.