https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&feed=atom&action=historyAstrophysical component separation - Revision history2024-03-29T05:19:06ZRevision history for this page on the wikiMediaWiki 1.31.6https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14225&oldid=prevBbarreir: /* SEVEM */2018-07-10T10:22:39Z<p><span dir="auto"><span class="autocomment">SEVEM</span></span></p>
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 10:22, 10 July 2018</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l37" >Line 37:</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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the cleaned CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the cleaned map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the cleaned maps.</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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the cleaned CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the cleaned map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the cleaned maps.</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 final CMB intensity map has then been constructed by combining the 143 and 217 GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100, 143 and 217 GHz cleaned maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps <del class="diffchange diffchange-inline">hava </del>been constructed at <i>N</i><sub>side</sub>=2048 <del class="diffchange diffchange-inline"> </del>and have a resolution of 5 arcmin.</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 final CMB intensity map has then been constructed by combining the 143 and 217 GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100, 143 and 217 GHz cleaned maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps <ins class="diffchange diffchange-inline">have </ins>been constructed at <i>N</i><sub>side</sub>=2048 and have a resolution of 5 arcmin.</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>===SMICA===</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>===SMICA===</div></td></tr>
</table>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14131&oldid=prevBbarreir: /* SEVEM */2018-07-06T15:49:59Z<p><span dir="auto"><span class="autocomment">SEVEM</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 15:49, 6 July 2018</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l32" >Line 32:</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</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 input maps used are all the Planck frequency channels. In the current release, we have cleaned the 70<del class="diffchange diffchange-inline">- </del>100<del class="diffchange diffchange-inline">-</del>, 143<del class="diffchange diffchange-inline">-</del>, and 217<del class="diffchange diffchange-inline">-</del>GHz maps for both intensity and polarization, at their native resolution. For intensity, we use the same four templates to clean the 100<del class="diffchange diffchange-inline">-</del>, 143<del class="diffchange diffchange-inline">- </del>and 217<del class="diffchange diffchange-inline">- </del>GHz. Three of them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz], [44GHz &ndash; 70GHz], and [545GHz &ndash; 353GHz], whereas the fourth template is given by the 857-GHz channel (smoothed  with the beam of the 545-GHz channel). In addition, we also clean the 70 GHz map using two templates, the [30GHz &ndash; 44GHz] difference map and a second template given as the difference [353GHz &ndash; 143GHz] constructed at the resolution of the 70 GHz map.</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 input maps used are all the Planck frequency channels. In the current release, we have cleaned the 70<ins class="diffchange diffchange-inline">, </ins>100, 143, and 217 GHz maps for both intensity and polarization, at their native resolution. For intensity, we use the same four templates to clean the 100, 143 and 217 GHz. Three of them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz], [44GHz &ndash; 70GHz], and [545GHz &ndash; 353GHz], whereas the fourth template is given by the 857-GHz channel (smoothed  with the beam of the 545-GHz channel). In addition, we also clean the 70 GHz map using two templates, the [30GHz &ndash; 44GHz] difference map and a second template given as the difference [353GHz &ndash; 143GHz] constructed at the resolution of the 70 GHz map.</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>For polarization, given the smaller number of frequency channels available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we inpaint the positions of point sources detected in the frequency maps, to reduce contamination in the final map.  </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>For polarization, given the smaller number of frequency channels available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we inpaint the positions of point sources detected in the frequency maps, to reduce contamination in the final map.  </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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the cleaned CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the cleaned map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the cleaned maps.</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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the cleaned CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the cleaned map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the cleaned maps.</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 final CMB intensity map has then been constructed by combining the 143<del class="diffchange diffchange-inline">- </del>and 217<del class="diffchange diffchange-inline">-</del>GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100<del class="diffchange diffchange-inline">-</del>, 143<del class="diffchange diffchange-inline">- </del>and 217<del class="diffchange diffchange-inline">-</del>GHz cleaned maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed at <i>N</i><sub>side</sub>=2048  and have a resolution of 5 arcmin.</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 final CMB intensity map has then been constructed by combining the 143 and 217 GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100, 143 and 217 GHz cleaned maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed at <i>N</i><sub>side</sub>=2048  and have a resolution of 5 arcmin.</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>===SMICA===</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>===SMICA===</div></td></tr>
</table>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14128&oldid=prevBbarreir: /* SEVEM */2018-07-06T15:41:19Z<p><span dir="auto"><span class="autocomment">SEVEM</span></span></p>
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 15:41, 6 July 2018</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;"></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>===SEVEM===</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>===SEVEM===</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><del class="diffchange diffchange-inline">Sevem </del>produces cleaned CMB maps at individual frequencies by using a procedure based on template fitting, which can then be combined to produce a final CMB map. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases ({{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}). In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.  </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">SEVEM </ins>produces cleaned CMB maps at individual frequencies by using a procedure based on template fitting, which can then be combined to produce a final CMB map. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases ({{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}). In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.  </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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</div></td></tr>
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</table>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14109&oldid=prevBbarreir: /* SEVEM */2018-07-06T13:41:21Z<p><span dir="auto"><span class="autocomment">SEVEM</span></span></p>
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</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l32" >Line 32:</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</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 input maps used are all the Planck frequency channels. In the current release, we have cleaned the 70- 100-, 143-, and 217-GHz maps for both intensity and polarization, at their native resolution. For intensity, we use the same four templates to clean the 100-, 143- and 217- GHz. Three of them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz]<del class="diffchange diffchange-inline">; </del>[44GHz &ndash; 70GHz]<del class="diffchange diffchange-inline">; </del>and [545GHz &ndash; 353GHz], whereas the fourth template is given by the 857-GHz channel (smoothed  with the beam of the 545-GHz channel). In addition, we also clean the 70 GHz map using two templates, the [30GHz &ndash; 44GHz] difference map and a second template given as the difference [353GHz &ndash; 143GHz] constructed at the resolution of the 70 GHz map.</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 input maps used are all the Planck frequency channels. In the current release, we have cleaned the 70- 100-, 143-, and 217-GHz maps for both intensity and polarization, at their native resolution. For intensity, we use the same four templates to clean the 100-, 143- and 217- GHz. Three of them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz]<ins class="diffchange diffchange-inline">, </ins>[44GHz &ndash; 70GHz]<ins class="diffchange diffchange-inline">, </ins>and [545GHz &ndash; 353GHz], whereas the fourth template is given by the 857-GHz channel (smoothed  with the beam of the 545-GHz channel). In addition, we also clean the 70 GHz map using two templates, the [30GHz &ndash; 44GHz] difference map and a second template given as the difference [353GHz &ndash; 143GHz] constructed at the resolution of the 70 GHz map.</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>For polarization, given the smaller number of frequency channels available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we inpaint the positions of point sources detected in the frequency maps, to reduce contamination in the final map.  </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>For polarization, given the smaller number of frequency channels available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we inpaint the positions of point sources detected in the frequency maps, to reduce contamination in the final map.  </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>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14076&oldid=prevBbarreir: /* SEVEM */2018-07-06T10:30:47Z<p><span dir="auto"><span class="autocomment">SEVEM</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 10:30, 6 July 2018</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l35" >Line 35:</td>
<td colspan="2" class="diff-lineno">Line 35:</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>For polarization, given the smaller number of frequency channels available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we inpaint the positions of point sources detected in the frequency maps, to reduce contamination in the final map.  </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>For polarization, given the smaller number of frequency channels available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we inpaint the positions of point sources detected in the frequency maps, to reduce contamination in the final map.  </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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the <del class="diffchange diffchange-inline">clean </del>CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the <del class="diffchange diffchange-inline">clean </del>map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the <del class="diffchange diffchange-inline">clean </del>maps.</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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the <ins class="diffchange diffchange-inline">cleaned </ins>CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the <ins class="diffchange diffchange-inline">cleaned </ins>map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the <ins class="diffchange diffchange-inline">cleaned </ins>maps.</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 final CMB intensity map has then been constructed by combining the 143- and 217-GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100-, 143- and 217-GHz cleaned maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed at <i>N</i><sub>side</sub>=2048  and have a resolution of 5 arcmin.</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 final CMB intensity map has then been constructed by combining the 143- and 217-GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100-, 143- and 217-GHz cleaned maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed at <i>N</i><sub>side</sub>=2048  and have a resolution of 5 arcmin.</div></td></tr>
<!-- diff cache key wiki_planck_legacy_archive:diff::1.12:old-14072:rev-14076 -->
</table>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14072&oldid=prevBbarreir: /* SEVEM */2018-07-06T10:28:59Z<p><span dir="auto"><span class="autocomment">SEVEM</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 10:28, 6 July 2018</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l32" >Line 32:</td>
<td colspan="2" class="diff-lineno">Line 32:</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</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 input maps used are all the Planck frequency channels. In the current release, we have cleaned the 70- 100-, 143-, and 217-GHz maps for both intensity and polarization, at their native resolution. For intensity, we use the same four templates to clean the 100-, 143- and 217- GHz. Three <del class="diffchange diffchange-inline">or </del>them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz]; [44GHz &ndash; 70GHz]; and [545GHz &ndash; 353GHz], whereas the fourth template is given by the 857-GHz channel (smoothed  <del class="diffchange diffchange-inline">at </del>the <del class="diffchange diffchange-inline">resolution </del>of the 545-GHz channel). In addition, we also clean the 70 GHz map using two templates, the [30GHz &ndash; 44GHz] difference map and a second template <del class="diffchange diffchange-inline">constructed </del>as the difference [353GHz &ndash; 143GHz] <del class="diffchange diffchange-inline">smoothed to </del>the resolution of the 70 GHz map.</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 input maps used are all the Planck frequency channels. In the current release, we have cleaned the 70- 100-, 143-, and 217-GHz maps for both intensity and polarization, at their native resolution. For intensity, we use the same four templates to clean the 100-, 143- and 217- GHz. Three <ins class="diffchange diffchange-inline">of </ins>them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz]; [44GHz &ndash; 70GHz]; and [545GHz &ndash; 353GHz], whereas the fourth template is given by the 857-GHz channel (smoothed  <ins class="diffchange diffchange-inline">with </ins>the <ins class="diffchange diffchange-inline">beam </ins>of the 545-GHz channel). In addition, we also clean the 70 GHz map using two templates, the [30GHz &ndash; 44GHz] difference map and a second template <ins class="diffchange diffchange-inline">given </ins>as the difference [353GHz &ndash; 143GHz] <ins class="diffchange diffchange-inline">constructed at </ins>the resolution of the 70 GHz map.</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>For polarization, given the <del class="diffchange diffchange-inline">lower range </del>of frequency <del class="diffchange diffchange-inline">maps </del>available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we <del class="diffchange diffchange-inline">perform inpainting at </del>the positions of <del class="diffchange diffchange-inline">detected </del>point sources to reduce contamination in the final map.  </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>For polarization, given the <ins class="diffchange diffchange-inline">smaller number </ins>of frequency <ins class="diffchange diffchange-inline">channels </ins>available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we <ins class="diffchange diffchange-inline">inpaint </ins>the positions of point sources <ins class="diffchange diffchange-inline">detected in the frequency maps, </ins>to reduce contamination in the final map.  </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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the clean CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the clean map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the clean maps.</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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the clean CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the clean map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the clean maps.</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 final CMB intensity map has then been constructed by combining the 143- and 217-GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100-, 143- and 217-GHz <del class="diffchange diffchange-inline">clean </del>maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed at <i>N</i><sub>side</sub>=2048  and have a resolution of 5 arcmin.</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 final CMB intensity map has then been constructed by combining the 143- and 217-GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100-, 143- and 217-GHz <ins class="diffchange diffchange-inline">cleaned </ins>maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed at <i>N</i><sub>side</sub>=2048  and have a resolution of 5 arcmin.</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>===SMICA===</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>===SMICA===</div></td></tr>
</table>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14070&oldid=prevBbarreir: /* SEVEM */2018-07-06T10:22:07Z<p><span dir="auto"><span class="autocomment">SEVEM</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 10:22, 6 July 2018</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l28" >Line 28:</td>
<td colspan="2" class="diff-lineno">Line 28:</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>===SEVEM===</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>===SEVEM===</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><del class="diffchange diffchange-inline">The aim of </del>Sevem <del class="diffchange diffchange-inline">is to produce clean </del>CMB maps at <del class="diffchange diffchange-inline">one or several </del>frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases ({{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}). In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust<del class="diffchange diffchange-inline">. Some of the cleaned maps are then combine to provide a final CMB map</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>Sevem <ins class="diffchange diffchange-inline">produces cleaned </ins>CMB maps at <ins class="diffchange diffchange-inline">individual </ins>frequencies by using a procedure based on template fitting<ins class="diffchange diffchange-inline">, which can then be combined to produce a final CMB map</ins>. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases ({{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}). In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.  </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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous one, although we provide now a cleaned 70 GHz map in intensity. However, for polarization, given the significant improvement in the quality of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combined map and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to that of a Gaussian beam of 5 arcminutes).</div></td></tr>
</table>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14067&oldid=prevBbarreir: /* SEVEM */2018-07-06T10:20:36Z<p><span dir="auto"><span class="autocomment">SEVEM</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 10:20, 6 July 2018</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l28" >Line 28:</td>
<td colspan="2" class="diff-lineno">Line 28:</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>===SEVEM===</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>===SEVEM===</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>The aim of Sevem is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases ({{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}). In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.</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 aim of Sevem is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases ({{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}). In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust<ins class="diffchange diffchange-inline">. Some of the cleaned maps are then combine to provide a final CMB map</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="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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to <del class="diffchange diffchange-inline">that of </del>the previous <del class="diffchange diffchange-inline">release</del>, although we provide now a cleaned 70 GHz in intensity. However, for polarization, given the <del class="diffchange diffchange-inline">large </del>improvement of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final <del class="diffchange diffchange-inline">combination </del>and, therefore, construct a <del class="diffchange diffchange-inline">final </del>CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to a Gaussian beam of 5 arcminutes).</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to the previous <ins class="diffchange diffchange-inline">one</ins>, although we provide now a cleaned 70 GHz <ins class="diffchange diffchange-inline">map </ins>in intensity. However, for polarization, given the <ins class="diffchange diffchange-inline">significant </ins>improvement <ins class="diffchange diffchange-inline">in the quality </ins>of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final <ins class="diffchange diffchange-inline">combined map </ins>and, therefore, construct a CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to <ins class="diffchange diffchange-inline">that of </ins>a Gaussian beam of 5 arcminutes).</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 input maps used are all the Planck frequency channels. In the current release, we have cleaned the 70- 100-, 143-, and 217-GHz maps for both intensity and polarization, at their native resolution. For intensity, we use the same four templates to clean the 100-, 143- and 217- GHz. Three or them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz]; [44GHz &ndash; 70GHz]; and [545GHz &ndash; 353GHz], whereas the fourth template is given by the 857-GHz channel (smoothed  at the resolution of the 545-GHz channel). In addition, we also clean the 70 GHz map using two templates, <del class="diffchange diffchange-inline">one given by </del>the <del class="diffchange diffchange-inline">same </del>[30GHz &ndash; 44GHz] difference map and a second <del class="diffchange diffchange-inline">one </del>constructed as the difference [353GHz &ndash; 143GHz] smoothed to the resolution of the 70 GHz map.</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 input maps used are all the Planck frequency channels. In the current release, we have cleaned the 70- 100-, 143-, and 217-GHz maps for both intensity and polarization, at their native resolution. For intensity, we use the same four templates to clean the 100-, 143- and 217- GHz. Three or them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz]; [44GHz &ndash; 70GHz]; and [545GHz &ndash; 353GHz], whereas the fourth template is given by the 857-GHz channel (smoothed  at the resolution of the 545-GHz channel). In addition, we also clean the 70 GHz map using two templates, the [30GHz &ndash; 44GHz] difference map and a second <ins class="diffchange diffchange-inline">template </ins>constructed as the difference [353GHz &ndash; 143GHz] smoothed to the resolution of the 70 GHz map.</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>For polarization, given the lower range of frequency maps available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we perform inpainting at the positions of detected point sources to reduce contamination in the final map.  </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>For polarization, given the lower range of frequency maps available, a different set of templates has to be chosen for each map. In particular, two templates are used to clean 70 GHz and three templates are considered for the rest of the frequencies (see Appendix C in {{PlanckPapers|planck2016-l04}} for details). Before constructing the templates, for both intensity and polarization, we perform inpainting at the positions of detected point sources to reduce contamination in the final map.  </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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the clean CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the clean map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the clean maps.</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>A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the clean CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the clean map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the clean maps.</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 final CMB intensity map has then been constructed by combining the 143- and 217-GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100-, 143-<del class="diffchange diffchange-inline">GHz </del>and 217-GHz clean maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed at <i>N</i><sub>side</sub>=2048  and have a resolution of 5 arcmin.</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 final CMB intensity map has then been constructed by combining the 143- and 217-GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100-, 143- and 217-GHz clean maps taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed at <i>N</i><sub>side</sub>=2048  and have a resolution of 5 arcmin.</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>===SMICA===</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>===SMICA===</div></td></tr>
</table>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14058&oldid=prevBbarreir: /* SEVEM */2018-07-06T09:38:01Z<p><span dir="auto"><span class="autocomment">SEVEM</span></span></p>
<table class="diff diff-contentalign-left" data-mw="interface">
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<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 09:38, 6 July 2018</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l28" >Line 28:</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;"></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>===SEVEM===</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>===SEVEM===</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>The aim of Sevem is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases {{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.</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 aim of Sevem is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases <ins class="diffchange diffchange-inline">(</ins>{{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}<ins class="diffchange diffchange-inline">)</ins>. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to that of the previous release, although we provide now a cleaned 70 GHz in intensity. However, for polarization, given the large improvement of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combination and, therefore, construct a final CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to a Gaussian beam of 5 arcminutes).</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>Regarding intensity, the pipeline for the 2018 release does not present any significant change with respect to that of the previous release, although we provide now a cleaned 70 GHz in intensity. However, for polarization, given the large improvement of the data, we are now able to clean robustly also the 217 GHz map which can be included in the final combination and, therefore, construct a final CMB map with better resolution and higher signal-to-noise. Thus, conversely to the 2015 release, the SEVEM polarization maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048, with a resolution equivalent to a Gaussian beam of 5 arcminutes).</div></td></tr>
</table>Bbarreirhttps://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Astrophysical_component_separation&diff=14057&oldid=prevBbarreir: /* CMB and foreground separation */2018-07-06T09:36:55Z<p><span dir="auto"><span class="autocomment">CMB and foreground separation</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 09:36, 6 July 2018</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;"></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>===SEVEM===</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>===SEVEM===</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>The aim of Sevem is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.</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 aim of Sevem is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008{{BibCite|leach2008}}), to WMAP polarization data (Fernandez-Cobos et al., 2012{{BibCite|fernandezcobos2012}}) and to the previous Planck data releases <ins class="diffchange diffchange-inline">{{PlanckPapers|planck2013-p06}}, {{PlanckPapers|planck2014-a11}}</ins>. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.</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><del class="diffchange diffchange-inline">The input maps used are all </del>the <del class="diffchange diffchange-inline">Planck frequency channels. In particular, in </del>the <del class="diffchange diffchange-inline">Planck </del>2018 release, we <del class="diffchange diffchange-inline">have </del>cleaned <del class="diffchange diffchange-inline">the </del>70<del class="diffchange diffchange-inline">- 100-, 143-, and 217-</del>GHz <del class="diffchange diffchange-inline">maps for both </del>intensity <del class="diffchange diffchange-inline">and polarization, at their native resolution</del>. <del class="diffchange diffchange-inline">For intensity</del>, <del class="diffchange diffchange-inline">we use the same four templates to clean the 100-</del>, <del class="diffchange diffchange-inline">143- and 217- GHz. Three or them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): [30GHz &ndash; 44GHz]; [44GHz &ndash; 70GHz]; and [545GHz &ndash; 353GHz], whereas the fourth template is </del>given <del class="diffchange diffchange-inline">by </del>the <del class="diffchange diffchange-inline">857-GHz channel (smoothed  at the resolution </del>of the <del class="diffchange diffchange-inline">545-GHz channel). In addition</del>, we also <del class="diffchange diffchange-inline">clean </del>the <del class="diffchange diffchange-inline">70 </del>GHz map <del class="diffchange diffchange-inline">using two templates, one given by </del>the <del class="diffchange diffchange-inline">same [30GHz &ndash; 44GHz] difference map </del>and <del class="diffchange diffchange-inline">a second one constructed as the difference [353GHz &ndash; 143GHz] smoothed to the resolution of the 70 GHz map.</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><ins class="diffchange diffchange-inline">Regarding intensity, </ins>the <ins class="diffchange diffchange-inline">pipeline for </ins>the 2018 <ins class="diffchange diffchange-inline">release does not present any significant change with respect to that of the previous </ins>release, <ins class="diffchange diffchange-inline">although </ins>we <ins class="diffchange diffchange-inline">provide now a </ins>cleaned 70 GHz <ins class="diffchange diffchange-inline">in </ins>intensity. <ins class="diffchange diffchange-inline">However</ins>, <ins class="diffchange diffchange-inline">for polarization</ins>, given the <ins class="diffchange diffchange-inline">large improvement </ins>of the <ins class="diffchange diffchange-inline">data</ins>, we <ins class="diffchange diffchange-inline">are now able to clean robustly </ins>also the <ins class="diffchange diffchange-inline">217 </ins>GHz map <ins class="diffchange diffchange-inline">which can be included in </ins>the <ins class="diffchange diffchange-inline">final combination </ins>and, <ins class="diffchange diffchange-inline">therefore</ins>, <ins class="diffchange diffchange-inline">construct </ins>a <ins class="diffchange diffchange-inline">final CMB map with better resolution and higher signal-</ins>to<ins class="diffchange diffchange-inline">-noise</ins>. <ins class="diffchange diffchange-inline">Thus</ins>, <ins class="diffchange diffchange-inline">conversely </ins>to the <ins class="diffchange diffchange-inline">2015 release, </ins>the <ins class="diffchange diffchange-inline">SEVEM </ins>polarization <ins class="diffchange diffchange-inline">maps are now provided at full resolution (<i>N</i><sub>side</sub>=2048</ins>, <ins class="diffchange diffchange-inline">with a resolution equivalent to a Gaussian beam </ins>of <ins class="diffchange diffchange-inline">5 arcminutes)</ins>.</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><del class="diffchange diffchange-inline">For polarization</del>, <del class="diffchange diffchange-inline">given the lower range of frequency maps available</del>, a <del class="diffchange diffchange-inline">different set of templates has </del>to <del class="diffchange diffchange-inline">be chosen</del>. <del class="diffchange diffchange-inline">In particular</del>, <del class="diffchange diffchange-inline">two templates are used </del>to <del class="diffchange diffchange-inline">clean 70 GHz and three templates are considered for </del>the <del class="diffchange diffchange-inline">rest of </del>the <del class="diffchange diffchange-inline">frequencies. Before constructing the templates, for both intensity and </del>polarization, <del class="diffchange diffchange-inline">we perform inpainting at the positions </del>of <del class="diffchange diffchange-inline">detected point sources to reduce contamination in the final map</del>.  </div></td><td colspan="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;"></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><del class="diffchange diffchange-inline">A linear combination of </del>the <del class="diffchange diffchange-inline">templates is then subtracted from </del>the <del class="diffchange diffchange-inline">Planck sky map </del>at the <del class="diffchange diffchange-inline">considered frequency</del>, <del class="diffchange diffchange-inline">in order </del>to <del class="diffchange diffchange-inline">produce </del>the <del class="diffchange diffchange-inline">clean </del>CMB <del class="diffchange diffchange-inline">map. The coefficients of </del>the <del class="diffchange diffchange-inline">linear combination are obtained </del>by <del class="diffchange diffchange-inline">minimizing </del>the <del class="diffchange diffchange-inline">variance </del>of the clean map <del class="diffchange diffchange-inline">outside </del>a given <del class="diffchange diffchange-inline">mask. Although we exclude very contaminated regions during </del>the <del class="diffchange diffchange-inline">minimization</del>, <del class="diffchange diffchange-inline">the subtraction is performed </del>for <del class="diffchange diffchange-inline">all pixels </del>and <del class="diffchange diffchange-inline">therefore </del>the <del class="diffchange diffchange-inline">cleaned maps cover </del>the <del class="diffchange diffchange-inline">full-sky </del>(<del class="diffchange diffchange-inline">although we expect that foreground residuals are present </del>in <del class="diffchange diffchange-inline">the excluded areas</del>). <del class="diffchange diffchange-inline">Inpainting </del>of point sources <del class="diffchange diffchange-inline">is also carried out </del>in the <del class="diffchange diffchange-inline">clean maps</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><ins class="diffchange diffchange-inline">The input maps used are all the Planck frequency channels. In </ins>the <ins class="diffchange diffchange-inline">current release, we have cleaned </ins>the <ins class="diffchange diffchange-inline">70- 100-, 143-, and 217-GHz maps for both intensity and polarization, </ins>at <ins class="diffchange diffchange-inline">their native resolution. For intensity, we use the same four templates to clean </ins>the <ins class="diffchange diffchange-inline">100-</ins>, <ins class="diffchange diffchange-inline">143- and 217- GHz. Three or them are constructed as the difference of the following Planck channels (smoothed to a common resolution </ins>to <ins class="diffchange diffchange-inline">remove </ins>the CMB <ins class="diffchange diffchange-inline">contribution): [30GHz &ndash; 44GHz]; [44GHz &ndash; 70GHz]; and [545GHz &ndash; 353GHz], whereas </ins>the <ins class="diffchange diffchange-inline">fourth template is given </ins>by the <ins class="diffchange diffchange-inline">857-GHz channel (smoothed  at the resolution </ins>of the <ins class="diffchange diffchange-inline">545-GHz channel). In addition, we also </ins>clean <ins class="diffchange diffchange-inline">the 70 GHz </ins>map <ins class="diffchange diffchange-inline">using two templates, one given by the same [30GHz &ndash; 44GHz] difference map and </ins>a <ins class="diffchange diffchange-inline">second one constructed as the difference [353GHz &ndash; 143GHz] smoothed to the resolution of the 70 GHz map.</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 class="diffchange diffchange-inline">For polarization, </ins>given the <ins class="diffchange diffchange-inline">lower range of frequency maps available</ins>, <ins class="diffchange diffchange-inline">a different set of templates has to be chosen </ins>for <ins class="diffchange diffchange-inline">each map. In particular, two templates are used to clean 70 GHz </ins>and <ins class="diffchange diffchange-inline">three templates are considered for </ins>the <ins class="diffchange diffchange-inline">rest of </ins>the <ins class="diffchange diffchange-inline">frequencies </ins>(<ins class="diffchange diffchange-inline">see Appendix C </ins>in <ins class="diffchange diffchange-inline">{{PlanckPapers|planck2016-l04}} for details</ins>). <ins class="diffchange diffchange-inline">Before constructing the templates, for both intensity and polarization, we perform inpainting at the positions </ins>of <ins class="diffchange diffchange-inline">detected </ins>point sources <ins class="diffchange diffchange-inline">to reduce contamination </ins>in the <ins class="diffchange diffchange-inline">final map</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="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 final CMB intensity map has then been constructed by combining the 143- and 217-GHz cleaned maps by weighting them <del class="diffchange diffchange-inline"> </del>in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100- and <del class="diffchange diffchange-inline">143</del>-GHz clean maps at <i>N</i><sub>side</sub>=<del class="diffchange diffchange-inline">1024 </del>and <del class="diffchange diffchange-inline">has </del>a resolution of <del class="diffchange diffchange-inline">10 </del>arcmin.</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">A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the clean CMB map. The coefficients of the linear combination are obtained by minimizing the variance of the clean map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and therefore the cleaned maps cover the full-sky (although, of course, foreground residuals are expected to be particularly large in the areas excluded in the minimisation). Inpainting of point sources is also carried out in the clean maps.</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> </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>The final CMB intensity map has then been constructed by combining the 143- and 217-GHz cleaned maps by weighting them in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcmin at <i>N</i><sub>side</sub>=2048. The final CMB polarization map has been obtained by combining the 100-<ins class="diffchange diffchange-inline">, 143-GHz </ins>and <ins class="diffchange diffchange-inline">217</ins>-GHz clean maps <ins class="diffchange diffchange-inline">taking into account the noise and resolution of each channel and suppressing the largest scales of the 217 GHz map, which are expected to be more affected by residual systematics. The Q/U maps hava been constructed </ins>at <i>N</i><sub>side</sub>=<ins class="diffchange diffchange-inline">2048  </ins>and <ins class="diffchange diffchange-inline">have </ins>a resolution of <ins class="diffchange diffchange-inline">5 </ins>arcmin.</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>===SMICA===</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>===SMICA===</div></td></tr>
</table>Bbarreir