Beam Window Functions

From Planck Legacy Archive Wiki
Revision as of 17:22, 15 February 2018 by Ehivon (talk | contribs)
Jump to: navigation, search

Beam window functions have computed with the Febecop Pipeline (as described here), and the QuickPol pipeline (see Hivon et al, 2017[1]). [2]

  1. QuickPol effective beam window functions

The beam window functions relate, over the full sky, or over a masked sky, the measured angular power spectrum (in the absence of noise) by a set of detectors, to the true underlying sky angular power spectrum (assumed to have isotropic statistical properties, as is the case for the CMB).

They are available in two forms:

  • a
  • b


  1. Hivon et al, 2017 "Quickpol"

Cosmic Microwave background