ABOUT LAMBDA

WMAP

The data made available through this page has been updated. The most recent version of this data may be accessed through /product/map/current/

Product Name
TE Power Spectrum
Mission
WMAP

Description

The angular power spectrum of the temperature-polarization correlations is computed using a quadratic estimator. ClTE is computed individually for each WMAP frequency band, using uniform weight for the temperature map and noise weight for the polarization maps. The power spectra are then combined using noise-weighted QVW data for l > 21 where foregrounds are insignificant, and a fit to CMB plus foregrounds using all five frequency bands for l ≤ 21.

The TE power spectrum data are provided as a table containing the following three columns:

  • the multipole moment l
  • the power spectrum in units of uK2
  • the corresponding diagonal elements of the covariance matrix

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.

A binned version of the TE power spectrum is also available in a separate file whose format and content are similar to those described above for the unbinned data. The choice of l bins is the same as that used in e.g., Figure 7 of Kogut et al. (see below).

More details can be found in:

"First Year Wilkinson Microwave Anisotropy Probe (WMAP) Results:
TE Polarization", Kogut, et al., 2003

WMAP Explanatory Supplement

Back to Product Page

A service of the HEASARC and of the Astrophysics Science Division at NASA/GSFC
Goddard Space Flight Center, National Aeronautics and Space Administration
HEASARC Director: Dr. Alan P. Smale
LAMBDA Director: Dr. Eric R. Switzer
NASA Official: Dr. Eric R. Switzer
Web Curator: Mr. Michael R. Greason