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The CMB has distinct peaks in both its temperature angular power spectrum(TT) and temperature-polarization cross-power spectrum (TE). From the WMAP datawe find the first peak in the temperature spectrum at l = 220.1 +- 0.8 with anamplitude of 74.7 +- 0.5 microK; the first trough at l = 411.7 +- 3.5 with anamplitude of 41.0 +- 0.5 microK; and the second peak at l = 546 +- 10 with anamplitude of 48.8 +- 0.9 microK. The TE spectrum has an antipeak at l = 137 +-9 with a cross-power of -35 +- 9 microK^2, and a peak at l = 329 +- 19 withcross-power 105 +- 18 microK^2. All uncertainties are 1 sigma and includecalibration and beam errors. An intuition for how the data determine thecosmological parameters may be gained by limiting one's attention to a subsetof parameters and their effects on the peak characteristics. We interpret thepeaks in the context of a flat adiabatic LambdaCDM model with the goal ofshowing how the cosmic baryon density, Omega_b h^2, matter density, Omega_mh^2, scalar index, n_s, and age of the universe are encoded in their positionsand amplitudes. To this end, we introduce a new scaling relation for the TEantipeak-to-peak amplitude ratio and recompute known related scaling relationsfor the TT spectrum in light of the WMAP data. From the scaling relations, weshow that WMAP's tight bound on Omega_b h^2 is intimately linked to its robustdetection of the first and second peaks of the TT spectrum.

First‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Interpretation of the TT and TE Angular Power Spectrum Peaks