Wilkinson Microwave Anisotropy Probe DR4
The data made available through this page has been updated. The most recent version of this data may be accessed through https://lambda.gsfc.nasa.gov/product/wmap/current/"
DR4 Polarization Power Spectra (includes binned versions)
The TE, TB, EE, and BB power spectra are computed using a pseudo-Cl estimatorfor the region outside the 5yr polarization mask in P and outside the analysis mask in T. Forthe temperature-polarization cross spectra (TE and TB), foreground-cleaned V and W bandsare used for T, foreground-cleaned Q, V, and W bands are used for polarization, and uniformweighting is used for multipole l <= 500, and Nobs weighting is used for l > 500. These TEand TB spectra are derived from data files released with version 4.1 of the WMAP likelihoodcode. The polarization auto spectra (EE and BB) also use foreground-cleaned Q, V, and Wbands, but they use uniform weighting at all l.
Unbinned TE, TB, EE, and BB power spectra are provided as tables containing the following columns:
The diagonal elements provide an estimate of the error, but should not be used as exact error bars. The complete Fisher matrix should be used for that purpose.
Binned versions of the TE, TB, EE, and BB power spectra are also available in separate ASCII files with the following columns:
The EE and BB spectra bins are noise-weighted averages; the TE and TBspectra bins are straight averages. The binned cross spectra (TE and TB) are given in the form
Also available are the BB power spectra before coadding frequences (Q, V, and W bands) as a table containing the following columns:
Like the other spectra, these are supplied in the form