# Difference between revisions of "L3 LFI"

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== Power Spectra == | == Power Spectra == | ||

− | LFI temperature power spectra are computed from frequency maps using | + | 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. | + | 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. |

The details can be found in {{PlanckPapers|planck2013-p02}} {{PlanckPapers|planck2014-a03||Planck-2015-A03}}. | The details can be found in {{PlanckPapers|planck2013-p02}} {{PlanckPapers|planck2014-a03||Planck-2015-A03}}. |

## Revision as of 13:45, 4 February 2015

## Power Spectra[edit]

LFI temperature power spectra are computed from frequency maps using cROMAster, an implementation of the pseudo- method described in^{[1]}, extended to derive both auto- and cross-power spectra^{[2]} 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 Planck-2013-IV^{[3]}Planck-2015-A05^{[4]}. Coupling kernels to correct for incomplete sky coverage are computed as described in Annex B of Planck-2013-XV^{[5]}Planck-2015-A13^{[6]}. We have masked the Galactic plane and point sources using masks described in Sec. 3 of Planck-2013-XII^{[7]}Planck-2015-A12^{[8]}. 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 Planck-2013-XV^{[5]}Planck-2015-A13^{[6]}when adding a simple foreground component to account for unresolved point source residuals at small angular scales.

The details can be found in Planck-2013-II^{[9]}Planck-2015-A03^{[10]}.

## References[edit]

- ↑
**MASTER of the Cosmic Microwave Background Anisotropy Power Spectrum: A Fast Method for Statistical Analysis of Large and Complex Cosmic Microwave Background Data Sets**, E. Hivon, K. M. Górski, C. B. Netterfield, B. P. Crill, S. Prunet, F. Hansen, ApJ,**567**, 2-17, (2002). - ↑
**Unbiased estimation of an angular power spectrum**, G. Polenta, D. Marinucci, A. Balbi, P. de Bernardis, E. Hivon, S. Masi, P. Natoli, N. Vittorio, J. Cosmology Astropart. Phys.,**11**, 1, (2005). - ↑
**Planck 2013 results. IV. Low Frequency Instrument beams and window functions**, Planck Collaboration, 2014, A&A, 571, A4 - ↑
**Planck 2015 results. IV. LFI beams and window functions**, Planck Collaboration, 2016, A&A, 594, A4. - ↑
^{5.0}^{5.1}**Planck 2013 results. XV. CMB power spectra and likelihood**, Planck Collaboration, 2014, A&A, 571, A15 - ↑
^{6.0}^{6.1}**Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of cosmological parameters**, Planck Collaboration, 2016, A&A, 594, A11. - ↑
**Planck 2013 results. XI. Component separation**, Planck Collaboration, 2014, A&A, 571, A11 - ↑
**Planck 2015 results. X. Diffuse component separation: Foreground maps**, Planck Collaboration, 2016, A&A, 594, A10. - ↑
**Planck 2013 results. II. Low Frequency Instrument data processing**, Planck Collaboration, 2014, A&A, 571, A2 - ↑
**Planck 2015 results. II. LFI processing**, Planck Collaboration, 2016, A&A, 594, A2.

(Planck) Low Frequency Instrument