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
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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|there]]), and
 
the QuickPol pipeline
 
the QuickPol pipeline
(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|2017A&A...598A..25H]]</ref>).
+
(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|2017A&A...598A..25H]]</ref>, and the 2018 Planck Likelihood paper).
 +
 
 +
The beam window functions relate, over the full sky or over a masked sky, the angular power spectrum measured (in the absence of noise) on a map produced
 +
by a set of detectors <math>C_{XX}^{map}(\ell)</math>, to the true underlying sky angular power spectrum <math>C_{XX}^{sky}(\ell)</math> (assumed to have isotropic statistical properties, as is the case for the CMB).
  
  
 
# QuickPol effective beam window functions
 
# 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:
 
They are available in two forms:
* The beam window function
+
* The beam window functions <math>b_{T}, b_{E}, b_{B},</math>
<math>b_{T}, b_{E}, b_{B},</math>
+
such that \\
such that  
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<math>C_{XX}^{map}(\ell) = b_{X}^2(\ell) w_{pix}^2(\ell) C_{XX}^{sky}(\ell)</math> \\
<math>C_{XX}^{map}(\ell) = b_{X}^2(\ell) w_{pix}^2(\ell) C_{XX}^{sky}(\ell)</math>  
+
for X=T,E or B, and where <math>w_{pix}</math> is the pixel window function, which depends on the resolution parameter Nside (=2048 for Planck HFI maps).
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
+
They are provided in FITS files, in a format compatible with [[http://healpix.sourceforge.net|HEALPix]]
 +
tools such as synfast and smoothing, as well as with PolSpice.
  
 
* Beam matrix
 
* Beam matrix

Revision as of 08:33, 16 February 2018

Beam window functions have computed with the Febecop Pipeline (as described there), and the QuickPol pipeline (see Hivon et al, 2017 [1], and the 2018 Planck Likelihood paper).

The beam window functions relate, over the full sky or over a masked sky, the angular power spectrum measured (in the absence of noise) on a map produced by a set of detectors [math]C_{XX}^{map}(\ell)[/math], to the true underlying sky angular power spectrum [math]C_{XX}^{sky}(\ell)[/math] (assumed to have isotropic statistical properties, as is the case for the CMB).


  1. QuickPol effective beam window functions

They are available in two forms:

  • The beam window functions [math]b_{T}, b_{E}, b_{B},[/math]

such that \\ [math]C_{XX}^{map}(\ell) = b_{X}^2(\ell) w_{pix}^2(\ell) C_{XX}^{sky}(\ell)[/math] \\ for X=T,E or B, and where [math]w_{pix}[/math] is the pixel window function, which depends on the resolution parameter Nside (=2048 for Planck HFI maps). They are provided in FITS files, in a format compatible with [[2]] tools such as synfast and smoothing, as well as with PolSpice.

  • Beam matrix

References[edit]

  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

(Planck) High Frequency Instrument

Flexible Image Transfer Specification