WMAP Angular Power Spectrum
Upper panel: SpICE measurement of the unbinned angular power spectrum (red line). Results from Hinshaw et al. 2003 (based on MASTER) are also shown (black line). Both measurements are in perfect agreement.
Lower panel: Binned angular power spectrum obtained with SpICE for two different sky cuts: Kp2 (red) & Kp0 (blue). It is in excellent agreement with measurements from Hinshaw et al. 2003 (black line) for virtually all multipoles < 700. Highest multipoles are still compatible within the errors.
Constraints for a 6 parameter spatially flat power-law LCDM model (we impose a prior, tau < 0.3), given our measurement of the WMAP angular power spectrum with SpICE and errors computed with the intra-bin variance (IBV) method (see paper for further details and best-fit values). 2D plots: Solid lines show the 68 and 95 % confidence intervals. 1D plots: solid lines are marginalised likelihoods. The 6D parameter covariance matrix for the obove plot is given below (entries in matrix follow order in base of triangle plot: baryon density, dark matter density, reionization optical depth, spectral index, sigma8, and Hubble constant). The covariance matrix can be used as proposal density to generate Markov Chains for WMAP. Chains, likelihoods and covariances have been computed using CosmoMC.
|Fosalba & Szapudi (2004), astro-ph/0405589||Binned Power Spectrum||6D Parameter Covariance Matrix|
|Unbinned Power Spectrum|