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 (see Hivon et al, 2017{{BibCite|hivon2017 | + | the QuickPol pipeline (see Hivon et al, 2017{{BibCite|hivon2017}}). |
| + | <ref>Hivon et al, 2017 "Quickpol" </ref> | ||
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* a | * a | ||
* b | * b | ||
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| + | === References === | ||
Revision as of 17:19, 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]). [2]
- 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]
Cosmic Microwave background
