# Difference between revisions of "Beam Window Functions"

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Beam window functions have computed with the Febecop Pipeline (as described [[Effective_Beams#Statistics_of_the_effective_beams_computed_using_FEBeCoP|here]]), and | Beam window functions have computed with the Febecop Pipeline (as described [[Effective_Beams#Statistics_of_the_effective_beams_computed_using_FEBeCoP|here]]), and | ||

the QuickPol pipeline | the QuickPol pipeline | ||

− | (see <ref>Hivon | + | (see Hivon et al, 2017 <ref>Hivon E., Mottet, S. & Ponthieu N., 2017 "QuickPol: Fast calculation of effective beam matrices for CMB polarization" A&A 598, A25, http://cdsads.u-strasbg.fr/abs/2017A&A...598A..25H</ref>). |

## Revision as of 17:30, 15 February 2018

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

### References[edit]

- ↑ Hivon E., Mottet, S. & Ponthieu N., 2017 "QuickPol: Fast calculation of effective beam matrices for CMB polarization" A&A 598, A25, http://cdsads.u-strasbg.fr/abs/2017A&A...598A..25H

Cosmic Microwave background