Difference between revisions of "L3 LFI"
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== Power Spectra == | == Power Spectra == | ||
| + | The TT, TE, and EE power spectra are described in [[CMB_spectrum_%26_Likelihood_Code | CMB spectrum]] section of the Products chapter. | ||
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LFI temperature power spectra are computed from frequency maps using cROMAster, an implementation of the pseudo-<math> C_\ell</math> method described in{{BibCite|master}}, extended to derive both auto- and cross-power spectra{{BibCite|polenta_CrossSpectra}} for a comparison between the two estimators. Noise bias and covariance matrices have been computed through the Full Focal Plane Simulations version 7 ''FFP7'', which includes 1000 realization of both signal and noise maps consistent with Planck data. The angular response of the instrument is accounted for by using the beam window functions presented in {{PlanckPapers|planck2013-p02d}} {{PlanckPapers|planck2014-a05||Planck-2015-A05}}. Coupling kernels to correct for incomplete sky coverage are computed as described in Annex B of {{PlanckPapers|planck2013-p08}} {{PlanckPapers|planck2014-a13||Planck-2015-A13}}. We have masked the Galactic plane and point sources using masks described in Sec. 3 of {{PlanckPapers|planck2013-p06}} {{PlanckPapers|planck2014-a12||Planck-2015-A12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, and the 60% Galactic mask for 30 GHz. | LFI temperature power spectra are computed from frequency maps using cROMAster, an implementation of the pseudo-<math> C_\ell</math> method described in{{BibCite|master}}, extended to derive both auto- and cross-power spectra{{BibCite|polenta_CrossSpectra}} for a comparison between the two estimators. Noise bias and covariance matrices have been computed through the Full Focal Plane Simulations version 7 ''FFP7'', which includes 1000 realization of both signal and noise maps consistent with Planck data. The angular response of the instrument is accounted for by using the beam window functions presented in {{PlanckPapers|planck2013-p02d}} {{PlanckPapers|planck2014-a05||Planck-2015-A05}}. Coupling kernels to correct for incomplete sky coverage are computed as described in Annex B of {{PlanckPapers|planck2013-p08}} {{PlanckPapers|planck2014-a13||Planck-2015-A13}}. We have masked the Galactic plane and point sources using masks described in Sec. 3 of {{PlanckPapers|planck2013-p06}} {{PlanckPapers|planck2014-a12||Planck-2015-A12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, and the 60% Galactic mask for 30 GHz. | ||
We report in Fig. 1 the 30, 44, and 70 GHz temperature power spectra. These have been produced from frequency maps without performing component separation. Nevertheless, there is a clear agreement between the observed spectra and the Planck Likelihood Code bestfit {{PlanckPapers|planck2013-p08}} {{PlanckPapers|planck2014-a13||Planck-2015-A13}}when adding a simple foreground component to account for unresolved point source residuals at small angular scales. | We report in Fig. 1 the 30, 44, and 70 GHz temperature power spectra. These have been produced from frequency maps without performing component separation. Nevertheless, there is a clear agreement between the observed spectra and the Planck Likelihood Code bestfit {{PlanckPapers|planck2013-p08}} {{PlanckPapers|planck2014-a13||Planck-2015-A13}}when adding a simple foreground component to account for unresolved point source residuals at small angular scales. | ||
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[[File:LFI_TTspectra_styleguide_final.jpg|thumb|center|500px|'''Figure 1. Temperature power spectra at 30, 44 and 70 GHz. Dashed lines correspond to the Planck Likelihood Code best-fit plus a foreground component to account for unresolved point sources.''']] | [[File:LFI_TTspectra_styleguide_final.jpg|thumb|center|500px|'''Figure 1. Temperature power spectra at 30, 44 and 70 GHz. Dashed lines correspond to the Planck Likelihood Code best-fit plus a foreground component to account for unresolved point sources.''']] | ||
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Latest revision as of 17:06, 4 February 2015
Power Spectra
The TT, TE, and EE power spectra are described in CMB spectrum section of the Products chapter.
