https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&feed=atom&action=historyL3 LFI - Revision history2024-03-28T13:12:30ZRevision history for this page on the wikiMediaWiki 1.31.6https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=11236&oldid=prevAgregori at 17:06, 4 February 20152015-02-04T17:06:54Z<p></p>
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 17:06, 4 February 2015</td>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">The TT, TE, and EE power spectra are described in [[CMB_spectrum_%26_Likelihood_Code | CMB spectrum]] section of the Products chapter.</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"><!--</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div> </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins class="diffchange diffchange-inline">--></ins></div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><!--</div></td></tr>
</table>Agregorihttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=11158&oldid=prevBpartrid: /* Power Spectra */2015-02-04T13:45:36Z<p><span dir="auto"><span class="autocomment">Power Spectra</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 13:45, 4 February 2015</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using <del class="diffchange diffchange-inline">a </del>cROMAster, <del class="diffchange diffchange-inline">a </del>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<del class="diffchange diffchange-inline">)</del>. Noise bias and covariance <del class="diffchange diffchange-inline">matrix </del>have been computed through the Full Focal Plane Simulations version 7 ''FFP7'', <del class="diffchange diffchange-inline">that include </del>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 <del class="diffchange diffchange-inline">uncompleted </del>sky coverage are computed as described in Annex<del class="diffchange diffchange-inline">. </del>B of {{PlanckPapers|planck2013-p08}} {{PlanckPapers|planck2014-a13||Planck-2015-A13}}. We have masked 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, <del class="diffchange diffchange-inline">while we have used </del>the 60% Galactic mask for 30 GHz.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using cROMAster, <ins class="diffchange diffchange-inline">an </ins>implementation of the pseudo-<math> C_\ell</math> method described in{{BibCite|master}}<ins class="diffchange diffchange-inline">, </ins>extended to derive both auto- and cross-power spectra{{BibCite|polenta_CrossSpectra}} for a comparison between the two estimators. Noise bias and covariance <ins class="diffchange diffchange-inline">matrices </ins>have been computed through the Full Focal Plane Simulations version 7 ''FFP7'', <ins class="diffchange diffchange-inline">which includes </ins>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 <ins class="diffchange diffchange-inline">incomplete </ins>sky coverage are computed as described in Annex B of {{PlanckPapers|planck2013-p08}} {{PlanckPapers|planck2014-a13||Planck-2015-A13}}. We have masked <ins class="diffchange diffchange-inline">the </ins>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, <ins class="diffchange diffchange-inline">and </ins>the 60% Galactic mask for 30 GHz.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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 <ins class="diffchange diffchange-inline">at small angular scales</ins>.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{PlanckPapers|planck2013-p02}} {{PlanckPapers|planck2014-a03||Planck-2015-A03}}.  </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{PlanckPapers|planck2013-p02}} {{PlanckPapers|planck2014-a03||Planck-2015-A03}}.  </div></td></tr>
</table>Bpartridhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=10984&oldid=prevAgregori: /* Power Spectra */2015-02-03T13:37:36Z<p><span dir="auto"><span class="autocomment">Power Spectra</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 13:37, 3 February 2015</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 7 ''FFP7'', that include 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}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{PlanckPapers|planck2013-p08}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{PlanckPapers|planck2013-p06}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 7 ''FFP7'', that include 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<ins class="diffchange diffchange-inline">}} {{PlanckPapers|planck2014-a05||Planck-2015-A05</ins>}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{PlanckPapers|planck2013-p08<ins class="diffchange diffchange-inline">}} {{PlanckPapers|planck2014-a13||Planck-2015-A13</ins>}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{PlanckPapers|planck2013-p06<ins class="diffchange diffchange-inline">}} {{PlanckPapers|planck2014-a12||Planck-2015-A12</ins>}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>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}} when adding a simple foreground component to account for unresolved point source residuals.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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<ins class="diffchange diffchange-inline">}} {{PlanckPapers|planck2014-a13||Planck-2015-A13</ins>}}when adding a simple foreground component to account for unresolved point source residuals.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{PlanckPapers|planck2013-p02}}.  </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{PlanckPapers|planck2013-p02<ins class="diffchange diffchange-inline">}} {{PlanckPapers|planck2014-a03||Planck-2015-A03</ins>}}.  </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td></tr>
</table>Agregorihttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=10182&oldid=prevAgregori: /* Power Spectra */2014-12-16T12:00:56Z<p><span dir="auto"><span class="autocomment">Power Spectra</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 12:00, 16 December 2014</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version <del class="diffchange diffchange-inline">6 </del>''<del class="diffchange diffchange-inline">FFP6</del>'', that include 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}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{PlanckPapers|planck2013-p08}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{PlanckPapers|planck2013-p06}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version <ins class="diffchange diffchange-inline">7 </ins>''<ins class="diffchange diffchange-inline">FFP7</ins>'', that include 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}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{PlanckPapers|planck2013-p08}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{PlanckPapers|planck2013-p06}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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}} when adding a simple foreground component to account for unresolved point source residuals.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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}} when adding a simple foreground component to account for unresolved point source residuals.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
</table>Agregorihttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=9305&oldid=prevLmendes: /* Power Spectra */2014-07-17T14:46:39Z<p><span dir="auto"><span class="autocomment">Power Spectra</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 14:46, 17 July 2014</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{PlanckPapers|planck2013-p08<del class="diffchange diffchange-inline">}} {{P2013|15</del>}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{<del class="diffchange diffchange-inline">BibCite</del>|planck2013-p06<del class="diffchange diffchange-inline">}} {{P2013|12</del>}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{PlanckPapers|planck2013-p08}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{<ins class="diffchange diffchange-inline">PlanckPapers</ins>|planck2013-p06}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>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<del class="diffchange diffchange-inline">}} {{P2013|15</del>}} when adding a simple foreground component to account for unresolved point source residuals.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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}} when adding a simple foreground component to account for unresolved point source residuals.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{PlanckPapers|planck2013-p02<del class="diffchange diffchange-inline">}} {{P2013|2</del>}}.  </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{PlanckPapers|planck2013-p02}}.  </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td></tr>
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</table>Lmendeshttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=9304&oldid=prevLmendes: /* Power Spectra */2014-07-17T14:45:24Z<p><span dir="auto"><span class="autocomment">Power Spectra</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 14:45, 17 July 2014</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{<del class="diffchange diffchange-inline">PLanckPapers</del>|planck2013-p08}} {{P2013|15}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{BibCite|planck2013-p06}} {{P2013|12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{<ins class="diffchange diffchange-inline">PlanckPapers</ins>|planck2013-p08}} {{P2013|15}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{BibCite|planck2013-p06}} {{P2013|12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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}} {{P2013|15}} when adding a simple foreground component to account for unresolved point source residuals.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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}} {{P2013|15}} when adding a simple foreground component to account for unresolved point source residuals.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{<del class="diffchange diffchange-inline">PLanckPapers</del>|planck2013-p02}} {{P2013|2}}.  </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{<ins class="diffchange diffchange-inline">PlanckPapers</ins>|planck2013-p02}} {{P2013|2}}.  </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td></tr>
</table>Lmendeshttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=9303&oldid=prevLmendes: /* Power Spectra */2014-07-17T14:45:06Z<p><span dir="auto"><span class="autocomment">Power Spectra</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 14:45, 17 July 2014</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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 {{<del class="diffchange diffchange-inline">BibCite</del>|planck2013-p02d<del class="diffchange diffchange-inline">}} {{P2013|4</del>}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{<del class="diffchange diffchange-inline">BibCite</del>|planck2013-p08}} {{P2013|15}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{BibCite|planck2013-p06}} {{P2013|12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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 {{<ins class="diffchange diffchange-inline">PlanckPapers</ins>|planck2013-p02d}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{<ins class="diffchange diffchange-inline">PLanckPapers</ins>|planck2013-p08}} {{P2013|15}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{BibCite|planck2013-p06}} {{P2013|12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>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 {{<del class="diffchange diffchange-inline">BibCite</del>|planck2013-p08}} {{P2013|15}} when adding a simple foreground component to account for unresolved point source residuals.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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 {{<ins class="diffchange diffchange-inline">PlanckPapers</ins>|planck2013-p08}} {{P2013|15}} when adding a simple foreground component to account for unresolved point source residuals.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{<del class="diffchange diffchange-inline">BibCite</del>|planck2013-p02}} {{P2013|2}}.  </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in {{<ins class="diffchange diffchange-inline">PLanckPapers</ins>|planck2013-p02}} {{P2013|2}}.  </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td></tr>
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</table>Lmendeshttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=9302&oldid=prevLmendes: /* Power Spectra */2014-07-17T14:43:47Z<p><span dir="auto"><span class="autocomment">Power Spectra</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
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<col class="diff-marker" />
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<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 14:43, 17 July 2014</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a implementation of the pseudo-<math> C_\ell</math> method described in {{BibCite|master}} extended to derive both auto- and cross-power spectra <del class="diffchange diffchange-inline">(see </del>{{BibCite|polenta_CrossSpectra}}<del class="diffchange diffchange-inline">) </del>for a comparison between the two estimators). Noise bias and covariance matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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 {{BibCite|planck2013-p02d}} {{P2013|4}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{BibCite|planck2013-p08}} {{P2013|15}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{BibCite|planck2013-p06}} {{P2013|12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a 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 matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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 {{BibCite|planck2013-p02d}} {{P2013|4}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of {{BibCite|planck2013-p08}} {{P2013|15}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of {{BibCite|planck2013-p06}} {{P2013|12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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 {{BibCite|planck2013-p08}} {{P2013|15}} when adding a simple foreground component to account for unresolved point source residuals.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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 {{BibCite|planck2013-p08}} {{P2013|15}} when adding a simple foreground component to account for unresolved point source residuals.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
</table>Lmendeshttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=9025&oldid=prevLmendes at 17:17, 4 June 20142014-06-04T17:17:08Z<p></p>
<table class="diff diff-contentalign-left" data-mw="interface">
<col class="diff-marker" />
<col class="diff-content" />
<col class="diff-marker" />
<col class="diff-content" />
<tr class="diff-title" lang="en-GB">
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 17:17, 4 June 2014</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td>
<td colspan="2" class="diff-lineno">Line 2:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Power Spectra ==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a implementation of the pseudo-<math> C_\ell</math> method described in <del class="diffchange diffchange-inline"><cite>#</del>master<del class="diffchange diffchange-inline"></cite> </del>extended to derive both auto- and cross-power spectra (see <del class="diffchange diffchange-inline"><cite>#</del>polenta_CrossSpectra<del class="diffchange diffchange-inline"></cite></del>) for a comparison between the two estimators). Noise bias and covariance matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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 <del class="diffchange diffchange-inline"><cite>#</del>planck2013-p02d<del class="diffchange diffchange-inline"></cite> </del>{{P2013|4}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of <del class="diffchange diffchange-inline"><cite>#</del>planck2013-p08<del class="diffchange diffchange-inline"></cite> </del>{{P2013|15}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of <del class="diffchange diffchange-inline"><cite>#</del>planck2013-p06<del class="diffchange diffchange-inline"></cite> </del>{{P2013|12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>LFI temperature power spectra are computed from frequency maps using a cROMAster, a implementation of the pseudo-<math> C_\ell</math> method described in <ins class="diffchange diffchange-inline">{{BibCite|</ins>master<ins class="diffchange diffchange-inline">}} </ins>extended to derive both auto- and cross-power spectra (see <ins class="diffchange diffchange-inline">{{BibCite|</ins>polenta_CrossSpectra<ins class="diffchange diffchange-inline">}}</ins>) for a comparison between the two estimators). Noise bias and covariance matrix have been computed through the Full Focal Plane Simulations version 6 ''FFP6'', that include 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 <ins class="diffchange diffchange-inline">{{BibCite|</ins>planck2013-p02d<ins class="diffchange diffchange-inline">}} </ins>{{P2013|4}}. Coupling kernels to correct for uncompleted sky coverage are computed as described in Annex. B of <ins class="diffchange diffchange-inline">{{BibCite|</ins>planck2013-p08<ins class="diffchange diffchange-inline">}} </ins>{{P2013|15}}. We have masked Galactic plane and point sources using masks described in Sec. 3 of <ins class="diffchange diffchange-inline">{{BibCite|</ins>planck2013-p06<ins class="diffchange diffchange-inline">}} </ins>{{P2013|12}}. In particular, we have used the 70% Galactic mask for 44 and 70 GHz, while we have used the 60% Galactic mask for 30 GHz.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>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 <del class="diffchange diffchange-inline"><cite>#</del>planck2013-p08<del class="diffchange diffchange-inline"></cite> </del>{{P2013|15}} when adding a simple foreground component to account for unresolved point source residuals.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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 <ins class="diffchange diffchange-inline">{{BibCite|</ins>planck2013-p08<ins class="diffchange diffchange-inline">}} </ins>{{P2013|15}} when adding a simple foreground component to account for unresolved point source residuals.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in <del class="diffchange diffchange-inline"><cite>#</del>planck2013-p02<del class="diffchange diffchange-inline"></cite> </del>{{P2013|2}}.  </div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The details can be found in <ins class="diffchange diffchange-inline">{{BibCite|</ins>planck2013-p02<ins class="diffchange diffchange-inline">}} </ins>{{P2013|2}}.  </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.''']]</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
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<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><del class="diffchange diffchange-inline">#[[References]]</del></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:LFI data processing|007]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:LFI data processing|007]]</div></td></tr>
</table>Lmendeshttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=L3_LFI&diff=8771&oldid=prevLmendes at 12:25, 21 May 20142014-05-21T12:25:40Z<p></p>
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</table>Lmendes