Beam Window Functions

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

  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:

  • The beam window function \

[math]b_{T}, b_{E}, b_{B},[/math]\

such that \

[math]C_{XX}^{map}(\ell) = b_{X}^2(\ell) w_pix(\ell)^2 C_{XX}^{sky}(\ell)[/math]\

for X=T,E or B, in FITS files, in a format compatible with HEALPix tools such as synfast and smoothing, as well as with PolSpice
  • Beam matrix


  1. Hivon E., Mottet, S. & Ponthieu N., 2017 QuickPol: Fast calculation of effective beam matrices for CMB polarization A&A 598, A25, [[1]]

Cosmic Microwave background

Flexible Image Transfer Specification

(Hierarchical Equal Area isoLatitude Pixelation of a sphere, <ref name="Template:Gorski2005">HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere, K. M. Górski, E. Hivon, A. J. Banday, B. D. Wandelt, F. K. Hansen, M. Reinecke, M. Bartelmann, ApJ, 622, 759-771, (2005).