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Diffuse component separation: CMB maps - CERN Document Server</title> <link href='https://framework.web.cern.ch/framework/2.0/fonts/PTSansWeb/PTSansWeb.css' rel='stylesheet' type='text/css' /> <link rel="stylesheet" href="https://cds.cern.ch/img/invenio.css?v=20141127" type="text/css" /> <link rel="stylesheet" href="https://cds.cern.ch/img/cern_theme/css/cern_theme.css?v=20141127" type="text/css" /> <link rel="stylesheet"href="/css/font-awesome.min.css"> <meta http-equiv="X-UA-Compatible" content="IE=Edge"/> <link rel="stylesheet" href="https://cds.cern.ch/img/cern_toolbar/css/toolbar.css" type="text/css" />    <link rel="canonical" href="https://cds.cern.ch/record/1993893/plots" /> <link rel="alternate" hreflang="el" href="https://cds.cern.ch/record/1993893/plots?ln=el" /> <link rel="alternate" hreflang="fr" href="https://cds.cern.ch/record/1993893/plots?ln=fr" /> <link rel="alternate" hreflang="bg" href="https://cds.cern.ch/record/1993893/plots?ln=bg" /> <link rel="alternate" hreflang="zh-TW" href="https://cds.cern.ch/record/1993893/plots?ln=zh_TW" /> <link rel="alternate" hreflang="pt" href="https://cds.cern.ch/record/1993893/plots?ln=pt" /> <link rel="alternate" hreflang="no" href="https://cds.cern.ch/record/1993893/plots?ln=no" /> <link rel="alternate" hreflang="hr" href="https://cds.cern.ch/record/1993893/plots?ln=hr" /> <link rel="alternate" hreflang="ca" href="https://cds.cern.ch/record/1993893/plots?ln=ca" /> <link rel="alternate" hreflang="de" href="https://cds.cern.ch/record/1993893/plots?ln=de" /> <link rel="alternate" hreflang="it" href="https://cds.cern.ch/record/1993893/plots?ln=it" /> <link rel="alternate" hreflang="zh-CN" href="https://cds.cern.ch/record/1993893/plots?ln=zh_CN" /> <link rel="alternate" hreflang="sv" href="https://cds.cern.ch/record/1993893/plots?ln=sv" /> <link rel="alternate" hreflang="sk" href="https://cds.cern.ch/record/1993893/plots?ln=sk" /> <link rel="alternate" hreflang="en" href="https://cds.cern.ch/record/1993893/plots?ln=en" /> <link rel="alternate" hreflang="pl" href="https://cds.cern.ch/record/1993893/plots?ln=pl" /> <link rel="alternate" hreflang="ru" href="https://cds.cern.ch/record/1993893/plots?ln=ru" /> <link rel="alternate" hreflang="ka" href="https://cds.cern.ch/record/1993893/plots?ln=ka" /> <link rel="alternate" hreflang="ja" href="https://cds.cern.ch/record/1993893/plots?ln=ja" /> <link rel="alternate" hreflang="es" href="https://cds.cern.ch/record/1993893/plots?ln=es" /> <link rel="alternate" type="application/rss+xml" title="CERN Document Server RSS" href="/rss?ln=en" /> <link rel="search" type="application/opensearchdescription+xml" href="https://cds.cern.ch/opensearchdescription" title="CERN Document Server" /> <link rel="unapi-server" type="application/xml" title="unAPI" href="https://cds.cern.ch/unapi" /> <link rel="apple-touch-icon" href="/apple-touch-icon.png"/> <link rel="apple-touch-icon-precomposed" href="/apple-touch-icon-precomposed.png"/> <meta http-equiv="Content-Type" content="text/html; charset=utf-8" /> <meta http-equiv="Content-Language" content="en" /> <meta name="description" content="We present foreground-reduced CMB maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales $\ell\gtrsim40$. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with $\ell < 20$ are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27$\,\mu\textrm{K}$ averaged over 55 arcmin pixels, and between 4.5 and 6.1$\,\mu\textrm{K}$ averaged over 3.4 arcmin pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the $1\sigma$ level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses. We present foreground-reduced cosmic microwave background (CMB) maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70GHz, and by 1.9 for frequencies between 100 and 857GHz. In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales l ≳ 40. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with l are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27muK averaged over 55' pixels, and between 4.5 and 6.1muK averaged over [??] pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the 1sigma level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses. However, the amplitude of primordial non-Gaussianity is consistent with zero within 2sigma for all local, equilateral, and orthogonal configurations of the bispectrum, including for polarization E-modes. Moreover, excellent agreement is found regarding the lensing B-mode power spectrum, both internally among the various component separation codes and with the best-fit Planck 2015 Lambda cold dark matter model. We present foreground-reduced CMB maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales $\ell\gtrsim40$. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with $\ell < 20$ are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27$\,\mu\textrm{K}$ averaged over 55 arcmin pixels, and between 4.5 and 6.1$\,\mu\textrm{K}$ averaged over 3.4 arcmin pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the $1\sigma$ level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses. Adam, R.; Ade, P.A.R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A.J.; Barreiro, R.B.; Bartlett, J.G.; Bartolo, N.; Basak, S.; Battaner, E.; Benabed, K.; Benoit, A.; Benoit-Levy, A.; Bernard, J.P.; Bersanelli, M.; Bielewicz, P.; Bonaldi, A.; Bonavera, L.; Bond, J.R.; Borrill, J.; Bouchet, F.R.; Boulanger, F.; Bucher, M.; Burigana, C.; Butler, R.C.; Calabrese, E.; Cardoso, J.F.; Casaponsa, B.; Castex, G.; Catalano, A.; Challinor, A.; Chamballu, A.; Chary, R.R.; Chiang, H.C.; Christensen, P.R.; Clements, D.L.; Colombi, S.; Colombo, L.P.L.; Combet, C.; Couchot, F.; Coulais, A.; Crill, B.P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R.D.; Davis, R.J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Desert, F.X.; Dickinson, C.; Diego, J.M.; Dole, H.; Donzelli, S.; Dore, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Ensslin, T.A.; Eriksen, H.K.; Falgarone, E.; Fantaye, Y.; Fergusson, J.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A.A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Ghosh, T.; Giard, M.; Giraud-Heraud, Y.; Gjerlow, E.; Gonzalez-Nuevo, J.; Gorski, K.M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J.E.; Hansen, F.K.; Hanson, D.; Harrison, D.L.; Helou, G.; Henrot-Versille, S.; Hernandez-Monteagudo, C.; Herranz, D.; Hildebrandt, S.R.; Hivon, E.; Hobson, M.; Holmes, W.A.; Hornstrup, A.; Hovest, W.; Huffenberger, K.M.; Hurier, G.; Jaffe, A.H.; Jaffe, T.R.; Jones, W.C.; Juvela, M.; Keihanen, E.; Keskitalo, R.; Kisner, T.S.; Kneissl, R.; Knoche, J.; Krachmalnicoff, N.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.M.; Lasenby, A.; Lattanzi, M.; Lawrence, C.R.; Le Jeune, M.; Leonardi, R.; Lesgourgues, J.; Levrier, F.; Liguori, M.; Lilje, P.B.; Linden-Vornle, M.; Lopez-Caniego, M.; Lubin, P.M.; Macias-Perez, J.F.; Maggio, G.; Maino, D.; Mandolesi, N.; Mangilli, A.; Marshall, D.J.; Martin, P.G.; Martinez-Gonzalez, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; McGehee, P.; Meinhold, P.R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschenes, M.A.; Molinari, D.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J.A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C.B.; Norgaard-Nielsen, H.U.; Noviello, F.; Novikov, D.; Novikov, I.; Oxborrow, C.A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Pasian, F.; Patanchon, G.; Pearson, T.J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Pratt, G.W.; Prezeau, G.; Prunet, S.; Puget, J.L.; Rachen, J.P.; Racine, B.; Reach, W.T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubino-Martin, J.A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Savini, G.; Scott, D.; Seiffert, M.D.; Shellard, E.P.S.; Spencer, L.D.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski, A.S.; Sygnet, J.F.; Tauber, J.A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Trombetti, T.; Tucci, M.; Tuovinen, J.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L.A.; Wandelt, B.D.; Wehus, I.K.; Yvon, D.; Zacchei, A.; Zonca, A." /> <meta name="keywords" content="CERN Document Server, WebSearch, CERN Document Server" /> <script type="text/javascript" src="https://cds.cern.ch/js/jquery.min.js"></script>  <link rel="stylesheet" href="https://cds.cern.ch/img/webnews.css" type="text/css" />  <script type="text/javascript" src="https://cds.cern.ch/js/webnews.js?v=20131009"></script> <meta property="fb:app_id" content="137353533001720"/> <script type="text/x-mathjax-config"> MathJax.Hub.Config({ tex2jax: {inlineMath: [['$','$']], processEscapes: true}, showProcessingMessages: false, messageStyle: "none" }); </script> <script src="/MathJax/MathJax.js?config=TeX-AMS_CHTML" type="text/javascript"> </script>  <meta content="Planck 2015 results. IX. Diffuse component separation: CMB maps" name="citation_title" /> <meta content="Adam, R." name="citation_author" /> <meta content="Wade, L.A." name="citation_author" /> <meta content="Stolyarov, V." name="citation_author" /> <meta content="Desert, F.X." name="citation_author" /> <meta content="Knoche, J." name="citation_author" /> <meta content="Giard, M." name="citation_author" /> <meta content="Dupac, X." name="citation_author" /> <meta content="Liguori, M." name="citation_author" /> <meta content="Matarrese, S." name="citation_author" /> <meta content="Kurki-Suonio, H." name="citation_author" /> <meta content="Mazzotta, P." name="citation_author" /> <meta content="Coulais, A." name="citation_author" /> <meta content="Gorski, K.M." name="citation_author" /> <meta content="Vielva, P." name="citation_author" /> <meta content="Gonzalez-Nuevo, J." name="citation_author" /> <meta content="Bucher, M." name="citation_author" /> <meta content="Reinecke, M." name="citation_author" /> <meta 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content="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_int_cmb_005a_2048.png" /> <meta property="og:image:secure_url" content="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_int_cmb_005a_2048.png" /> <meta property="og:image" content="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_hrhd_B-crop.png" /> <meta property="og:image:secure_url" content="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_hrhd_B-crop.png" /> <meta property="og:image" content="https://cds.cern.ch/record/1993893/files/figs_smica_filterEB_dx11.png" /> <meta property="og:image:secure_url" content="https://cds.cern.ch/record/1993893/files/figs_smica_filterEB_dx11.png" /> <meta content="CERN Document Server" property="og:site_name" /> <meta content="arXiv" property="og:description" /> <meta content="We present foreground-reduced CMB maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales $\ell\gtrsim40$. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with $\ell &lt; 20$ are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27$\,\mu\textrm{K}$ averaged over 55 arcmin pixels, and between 4.5 and 6.1$\,\mu\textrm{K}$ averaged over 3.4 arcmin pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the $1\sigma$ level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses." property="og:description" /> <meta content="We present foreground-reduced cosmic microwave background (CMB) maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70GHz, and by 1.9 for frequencies between 100 and 857GHz. In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales l ≳ 40. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with l are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27muK averaged over 55' pixels, and between 4.5 and 6.1muK averaged over [??] pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the 1sigma level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses. However, the amplitude of primordial non-Gaussianity is consistent with zero within 2sigma for all local, equilateral, and orthogonal configurations of the bispectrum, including for polarization E-modes. Moreover, excellent agreement is found regarding the lensing B-mode power spectrum, both internally among the various component separation codes and with the best-fit Planck 2015 Lambda cold dark matter model." property="og:description" /> <meta content="EDP Sciences" property="og:description" />  <meta content="summary" name="twitter:card" /> <style></style> </head> <body class="CERN32Document32Server search" lang="en">  <div id="cern-toolbar"> <h1><a href="http://cern.ch" title="CERN">CERN <span>Accelerating science</span></a></h1> <ul> <li class="cern-accountlinks"><a class="cern-account" href="https://cds.cern.ch/youraccount/login?ln=en&referer=https%3A//cds.cern.ch/record/1993893/plots" title="Sign in to your CERN account">Sign in</a></li> <li><a class="cern-directory" href="http://cern.ch/directory" title="Search CERN resources and browse the directory">Directory</a></li> </ul> </div>   <div role="banner" class="clearfix" id="header"> <div class="header-inner inner"> <hgroup class="clearfix"> <h2 id="site-name"> <a rel="home" title="Home" href="/"><span>CERN Document Server</span></a> </h2> <h3 id="site-slogan">Access articles, reports and multimedia content in HEP</h3> </hgroup> <div role="navigation" id="main-navigation" class="cdsmenu"> <h2 class="element-invisible">Main menu</h2><ul class="links inline clearfix"> <li class="menu-386 first active-trail"><a class="active-trail" href="https://cds.cern.ch/?ln=en">Search</a></li> <li class="menu-444 "><a class="" title="" href="https://cds.cern.ch/submit?ln=en">Submit</a></li> <li class="menu-426 "><a class="" href="https://cds.cern.ch/help/?ln=en">Help</a></li> <li class="leaf hassubcdsmenu"> <a hreflang="en" class="header" href="https://cds.cern.ch/youraccount/display?ln=en">Personalize</a> <ul class="subsubcdsmenu"><li><a href="https://cds.cern.ch/youralerts/list?ln=en">Your alerts</a></li><li><a href="https://cds.cern.ch/yourbaskets/display?ln=en">Your baskets</a></li><li><a href="https://cds.cern.ch/yourcomments?ln=en">Your comments</a></li><li><a href="https://cds.cern.ch/youralerts/display?ln=en">Your searches</a></li></ul></li> </ul> </div> </div> </div>  <table class="navtrailbox"> <tr> <td class="navtrailboxbody"> <a href="/?ln=en" class="navtrail">Home</a> > <a class="navtrail" href="/record/1993893">Planck 2015 results. IX. Diffuse component separation: CMB maps</a> > Plots </td> </tr> </table> </div> <div class="pagebody"><div class="pagebodystripemiddle"> <div class="detailedrecordbox"> <div class="detailedrecordtabs"> <div> <ul class="detailedrecordtabs"><li class="first"><a href="/record/1993893/?ln=en">Information </a></li><li class=""><a href="/record/1993893/files?ln=en">Files </a></li></ul> <div id="tabsSpacer" style="clear:both;height:0px"> </div></div> </div> <div class="detailedrecordboxcontent"> <div class="top-left-folded"></div> <div class="top-right-folded"></div> <div class="inside">  <div id="detailedrecordshortreminder"> <div id="clip"> </div> <div id="HB"> <strong><a href="/record/1993893?ln=en">Planck 2015 results. IX. Diffuse component separation: CMB maps</a></strong> - <a href="/search?f=author&p=Adam%2C%20R.&ln=en">Adam, R.</a> <em>et al</em> - arXiv:1502.05956 </div> </div> <div style="clear:both;height:1px"> </div> <table width="95%" style="display: inline;"><tr><td width="66%"><a name="0" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_common_int_mask_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_common_int_mask_005a_2048.png" width="95%"/></a></td><td width="33%"> Preferred masks for analysing component-separated CMB maps in temperature (\emph{left}) and polarization (\emph{right}).</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="1" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_common_pol_mask_new_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_common_pol_mask_new_010a_1024.png" width="95%"/></a></td><td width="33%"> Preferred masks for analysing component-separated CMB maps in temperature (\emph{left}) and polarization (\emph{right}).</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="2" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_commander_int_cmb_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_commander_int_cmb_005a_2048.png" width="95%"/></a></td><td width="33%"> Component-separated CMB temperature maps at full resolution, FWHM 5\arcm, $\nside = 2048$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="3" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_int_cmb_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_int_cmb_005a_2048.png" width="95%"/></a></td><td width="33%"> Differences between the component-separated CMB temperature maps from the 2013 and the 2015 releases. The maps have been smoothed to FWHM 80\arcm\ and downgrading to $\nside = 128$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="4" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_int_cmb_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_int_cmb_005a_2048.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="5" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_int_cmb_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_int_cmb_005a_2048.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="6" href="https://cds.cern.ch/record/1993893/files/figs_colourbar_300uK.png"><img src="https://cds.cern.ch/record/1993893/files/figs_colourbar_300uK.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="7" href="https://cds.cern.ch/record/1993893/files/figs_commander_diff_2013-2014_80arcmin_nomono.png"><img src="https://cds.cern.ch/record/1993893/files/figs_commander_diff_2013-2014_80arcmin_nomono.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="8" href="https://cds.cern.ch/record/1993893/files/figs_nilc_diff_2013-2014_80arcmin_nomono.png"><img src="https://cds.cern.ch/record/1993893/files/figs_nilc_diff_2013-2014_80arcmin_nomono.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="9" href="https://cds.cern.ch/record/1993893/files/figs_sevem_diff_2013-2014_80arcmin_nomono.png"><img src="https://cds.cern.ch/record/1993893/files/figs_sevem_diff_2013-2014_80arcmin_nomono.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="10" href="https://cds.cern.ch/record/1993893/files/figs_smica_diff_2013-2014_80arcmin_nomono.png"><img src="https://cds.cern.ch/record/1993893/files/figs_smica_diff_2013-2014_80arcmin_nomono.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="11" href="https://cds.cern.ch/record/1993893/files/figs_colourbar_15uK.png"><img src="https://cds.cern.ch/record/1993893/files/figs_colourbar_15uK.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="12" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_commander_nilc_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_commander_nilc_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between CMB temperature maps. As in the previous Fig.~\ref{fig:2015_2013_diff_I}, the maps have been smoothed to FWHM 80\arcm\ and downgraded to $\nside =128$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="13" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_commander_sevem_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_commander_sevem_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Difference between output and input CMB temperature maps from FFP8 simulations. Smoothing and downgrading as in Fig.~\ref{fig:dx11_diff_I}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="14" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_commander_smica_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_commander_smica_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="15" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_nilc_sevem_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_nilc_sevem_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="16" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_nilc_smica_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_nilc_smica_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="17" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_sevem_smica_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_int_sevem_smica_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="18" href="https://cds.cern.ch/record/1993893/files/figs_colourbar_7_5uK.png"><img src="https://cds.cern.ch/record/1993893/files/figs_colourbar_7_5uK.png" width="95%"/></a></td><td width="33%"> Caption not extractedPairwise difference maps between CMB temperature maps obtained on FFP8 simulations. Prior to differencing, the maps have been smoothed to 80 arcminutes FWHM and downgraded to N$_{side}$ = 128.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="19" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_commander_input_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_commander_input_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="20" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_nilc_input_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_nilc_input_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="21" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_sevem_input_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_sevem_input_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="22" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_smica_input_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_smica_input_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="23" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_commander_Q_case1_cmb_hp_20_40_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_commander_Q_case1_cmb_hp_20_40_010a_1024.png" width="95%"/></a></td><td width="33%"> Component-separated CMB $Q$ maps at resolution FWHM 10\arcm, $\nside = 1024$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="24" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_Q_case1_cmb_hp_20_40_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_Q_case1_cmb_hp_20_40_010a_1024.png" width="95%"/></a></td><td width="33%"> Component-separated CMB $U$ maps at resolution FWHM 10\arcm, $\nside = 1024$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="25" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_Q_case1_cmb_hp_20_40_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_Q_case1_cmb_hp_20_40_010a_1024.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="26" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_Q_case1_cmb_hp_20_40_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_Q_case1_cmb_hp_20_40_010a_1024.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="27" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_commander_U_case1_cmb_hp_20_40_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_commander_U_case1_cmb_hp_20_40_010a_1024.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="28" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_U_case1_cmb_hp_20_40_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_U_case1_cmb_hp_20_40_010a_1024.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="29" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_U_case1_cmb_hp_20_40_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_U_case1_cmb_hp_20_40_010a_1024.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="30" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_U_case1_cmb_hp_20_40_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_U_case1_cmb_hp_20_40_010a_1024.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="31" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_full_Q-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_full_Q-crop.png" width="95%"/></a></td><td width="33%"> $20\deg\times20\deg$ patch of the high-pass filtered \commander\ CMB polarization map, centered on the North Ecliptic Pole, $(l,b)=(96\deg,30\deg)$. Each map is pixelized with a \healpix\ resolution of $\nside=1024$, and has an angular resolution of $10\arcm$ FWHM. The top row shows $Q$ and $U$ maps derived from the full-mission data set, the middle row shows the corresponding $E$ and $B$ maps, and the bottom row shows the $E$ and $B$ maps of the half-ring half-difference (HRHD) map. Note the characteristic $+$ and $\times$ patterns in the $Q$ and $U$ maps, and the clear asymmetry between $E$ and $B$ in the full data set. Also note that the HRHD $E$ map is consistent with both the full and HRHD $B$ maps.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="32" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_full_U-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_full_U-crop.png" width="95%"/></a></td><td width="33%"> $20\deg\times20\deg$ patch of the high-pass filtered \commander\ CMB polarization map, centered on the North Ecliptic Pole, $(l,b)=(96\deg,30\deg)$. Each map is pixelized with a \healpix\ resolution of $\nside=1024$, and has an angular resolution of $10\arcm$ FWHM. The top row shows $Q$ and $U$ maps derived from the full-mission data set, the middle row shows the corresponding $E$ and $B$ maps, and the bottom row shows the $E$ and $B$ maps of the half-ring half-difference (HRHD) map. Note the characteristic $+$ and $\times$ patterns in the $Q$ and $U$ maps, and the clear asymmetry between $E$ and $B$ in the full data set. Also note that the HRHD $E$ map is consistent with both the full and HRHD $B$ maps.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="33" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_full_E-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_full_E-crop.png" width="95%"/></a></td><td width="33%"> $20\deg\times20\deg$ patch of the high-pass filtered \commander\ CMB polarization map, centered on the North Ecliptic Pole, $(l,b)=(96\deg,30\deg)$. Each map is pixelized with a \healpix\ resolution of $\nside=1024$, and has an angular resolution of $10\arcm$ FWHM. The top row shows $Q$ and $U$ maps derived from the full-mission data set, the middle row shows the corresponding $E$ and $B$ maps, and the bottom row shows the $E$ and $B$ maps of the half-ring half-difference (HRHD) map. Note the characteristic $+$ and $\times$ patterns in the $Q$ and $U$ maps, and the clear asymmetry between $E$ and $B$ in the full data set. Also note that the HRHD $E$ map is consistent with both the full and HRHD $B$ maps.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="34" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_full_B-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_full_B-crop.png" width="95%"/></a></td><td width="33%"> $20\deg\times20\deg$ patch of the high-pass filtered \commander\ CMB polarization map, centered on the North Ecliptic Pole, $(l,b)=(96\deg,30\deg)$. Each map is pixelized with a \healpix\ resolution of $\nside=1024$, and has an angular resolution of $10\arcm$ FWHM. The top row shows $Q$ and $U$ maps derived from the full-mission data set, the middle row shows the corresponding $E$ and $B$ maps, and the bottom row shows the $E$ and $B$ maps of the half-ring half-difference (HRHD) map. Note the characteristic $+$ and $\times$ patterns in the $Q$ and $U$ maps, and the clear asymmetry between $E$ and $B$ in the full data set. Also note that the HRHD $E$ map is consistent with both the full and HRHD $B$ maps.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="35" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_hrhd_E-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_hrhd_E-crop.png" width="95%"/></a></td><td width="33%"> $20\deg\times20\deg$ patch of the high-pass filtered \commander\ CMB polarization map, centered on the North Ecliptic Pole, $(l,b)=(96\deg,30\deg)$. Each map is pixelized with a \healpix\ resolution of $\nside=1024$, and has an angular resolution of $10\arcm$ FWHM. The top row shows $Q$ and $U$ maps derived from the full-mission data set, the middle row shows the corresponding $E$ and $B$ maps, and the bottom row shows the $E$ and $B$ maps of the half-ring half-difference (HRHD) map. Note the characteristic $+$ and $\times$ patterns in the $Q$ and $U$ maps, and the clear asymmetry between $E$ and $B$ in the full data set. Also note that the HRHD $E$ map is consistent with both the full and HRHD $B$ maps.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="36" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_hrhd_B-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_NEP_hrhd_B-crop.png" width="95%"/></a></td><td width="33%"> $20\deg\times20\deg$ patch of the high-pass filtered \commander\ CMB polarization map, centered on the North Ecliptic Pole, $(l,b)=(96\deg,30\deg)$. Each map is pixelized with a \healpix\ resolution of $\nside=1024$, and has an angular resolution of $10\arcm$ FWHM. The top row shows $Q$ and $U$ maps derived from the full-mission data set, the middle row shows the corresponding $E$ and $B$ maps, and the bottom row shows the $E$ and $B$ maps of the half-ring half-difference (HRHD) map. Note the characteristic $+$ and $\times$ patterns in the $Q$ and $U$ maps, and the clear asymmetry between $E$ and $B$ in the full data set. Also note that the HRHD $E$ map is consistent with both the full and HRHD $B$ maps.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="37" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_commander_nilc_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_commander_nilc_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $Q$ maps, after smoothing to FWHM 80\arcm\ and downgrading to $\nside = 128$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="38" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_commander_sevem_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_commander_sevem_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $Q$ maps, after smoothing to FWHM 80\arcm\ and downgrading to $\nside = 128$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="39" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_commander_smica_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_commander_smica_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $Q$ maps, after smoothing to FWHM 80\arcm\ and downgrading to $\nside = 128$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="40" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_nilc_sevem_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_nilc_sevem_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $Q$ maps, after smoothing to FWHM 80\arcm\ and downgrading to $\nside = 128$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="41" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_nilc_smica_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_nilc_smica_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $Q$ maps, after smoothing to FWHM 80\arcm\ and downgrading to $\nside = 128$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="42" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_sevem_smica_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_Q_sevem_smica_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $Q$ maps, after smoothing to FWHM 80\arcm\ and downgrading to $\nside = 128$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="43" href="https://cds.cern.ch/record/1993893/files/figs_colourbar_1uK.png"><img src="https://cds.cern.ch/record/1993893/files/figs_colourbar_1uK.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $Q$ maps, after smoothing to FWHM 80\arcm\ and downgrading to $\nside = 128$.Pairwise differences between CMB $U$ maps, after smoothing and downgrading as in Fig.~\ref{fig:dx11_diff_Q}.Caption not extractedPairwise difference maps between $Q$ maps obtained on FFP8 siulations. Smoothing and degrading as in Fig.~\ref{fig:dx11_diff_I}.Pairwise difference maps between $U$ maps obtained on FFP8 siulations. Smoothing and degrading as in Figs.~\ref{fig:dx11_diff_I},\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="44" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_commander_nilc_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_commander_nilc_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $U$ maps, after smoothing and downgrading as in Fig.~\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="45" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_commander_sevem_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_commander_sevem_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $U$ maps, after smoothing and downgrading as in Fig.~\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="46" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_commander_smica_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_commander_smica_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $U$ maps, after smoothing and downgrading as in Fig.~\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="47" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_nilc_sevem_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_nilc_sevem_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $U$ maps, after smoothing and downgrading as in Fig.~\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="48" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_nilc_smica_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_nilc_smica_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $U$ maps, after smoothing and downgrading as in Fig.~\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="49" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_sevem_smica_case1_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_diff_U_sevem_smica_case1_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise differences between CMB $U$ maps, after smoothing and downgrading as in Fig.~\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="50" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_commander_input_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_commander_input_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Difference between output and input CMB $Q$ maps from FFP8 simulations. Smoothing and downgrading as in Figs.~\ref{fig:dx11_diff_Q} and \ref{fig:dx11_diff_U}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="51" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_nilc_input_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_nilc_input_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Difference between output and input CMB $U$ maps from FFP8 simulations. Smoothing and downgrading as in Fig.~\ref{fig:ffp8_res_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="52" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_sevem_input_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_sevem_input_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="53" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_smica_input_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_smica_input_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="54" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_commander_input_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_commander_input_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="55" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_nilc_input_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_nilc_input_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="56" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_sevem_input_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_sevem_input_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="57" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_smica_input_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_smica_input_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="58" href="https://cds.cern.ch/record/1993893/files/figs_dx11_spec_raw_TT_cropped.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_spec_raw_TT_cropped.png" width="95%"/></a></td><td width="33%"> Power spectra of the the foreground-cleaned CMB maps. \textit{Left}: $TT$ power spectra evaluated using the \texttt{UT78} mask. \textit{Right}: $EE$ power spectra evaluated using the \texttt{UP78} mask. The thick lines show the spectra of the half-mission half-sum maps containing signal and noise. The thin lines show the spectra of the half-mission half-difference maps, which given an estimate of the noise. The black line shows the \Planck\ 2015 best-fit CMB spectrum for comparison.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="59" href="https://cds.cern.ch/record/1993893/files/figs_dx11_spec_raw_EE_cropped.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_spec_raw_EE_cropped.png" width="95%"/></a></td><td width="33%"> CMB $TT$ (\emph{left}) and $EE$ (\emph{right}) power spectra for each of the four foreground-cleaned maps. Top panels show raw bandpowers with no subtraction of extragalactic foregrounds; the grey lines show the best-fit \LCDM\ model from the \Planck\ 2015 likelihood. The bottom panels show residual bandpowers after subtracting the best-fit \LCDM\ model showing the residual extragalactic foreground contribution. The foregrounds are modelled and marginalized over when estimating parameters, see Figure~\ref{fig:dx11_params_TT_EE}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="60" href="https://cds.cern.ch/record/1993893/files/figs_dx11_spec_TT_cropped.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_spec_TT_cropped.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="61" href="https://cds.cern.ch/record/1993893/files/figs_dx11_spec_EE_cropped.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_spec_EE_cropped.png" width="95%"/></a></td><td width="33%"> Caption not extracted</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="62" href="https://cds.cern.ch/record/1993893/files/figs_dx11_par_TT_EE_cropped.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_par_TT_EE_cropped.png" width="95%"/></a></td><td width="33%"> Comparison of cosmological parameters estimated from the $TT$ and $EE$ spectra computed from the foreground-cleaned CMB maps. Within each group, the three left-most points show results for $TT$ with $\ell_{\mathrm{max}} = 1000$, $1500$, and $2000$ the two right-most points show results for $EE$ with $\ell_{\mathrm{max}} = 1000$ and $1500$. For comparison, we also show the corresponding parameters obtained with the \Planck\ 2015 likelihood including multipoles up to $\ell_{\mathrm{max}} = 2500$ as the horizontal line surrounded by a grey band giving the uncertainties. The foreground model used for the cleaned CMB maps is the method-tailored full-sky model from the FFP8 simulations.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="63" href="https://cds.cern.ch/record/1993893/files/figs_VarSkeKur_common_new_components4_cropped.png"><img src="https://cds.cern.ch/record/1993893/files/figs_VarSkeKur_common_new_components4_cropped.png" width="95%"/></a></td><td width="33%"> Polarised intensity variance (\emph{left column}), skewness (\emph{middle column}), and kurtosis (\emph{right column}) evaluated from the FFP8 Monte Carlo simulations (histogram) and from components of the fiducial FFP8 map at $\nside = 1024$ outside the \texttt{FFP8-UPA76} mask. The variance distributions have been normalized to the mean value of the Monte Carlo distributions for visualization purposes. Coloured vertical lines correspond to different combinations of components: the sum of CMB and noise is shown in blue; the sum of CMB, noise, and thermal dust is shown in green; the sum of CMB, noise, and radio point sources is shown in orange; the sum of CMB, noise, and all foregrounds is shown in red.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="64" href="https://cds.cern.ch/record/1993893/files/figs_variance_P_maps_new_common2_cropped.png"><img src="https://cds.cern.ch/record/1993893/files/figs_variance_P_maps_new_common2_cropped.png" width="95%"/></a></td><td width="33%"> Polarized intensity variance evaluated from the FFP8 Monte Carlo simulations (histogram) and from the \Planck\ 2015 maps (vertical red lines) outside the \texttt{UPB77} mask. Columns from left to right show different resolutions ($\nside = 1024$, $256$, and $64$), while rows show results for the four component separation methods. Unlike in Fig.~\ref{Fig:onepointsinglecomp}, the variance distributions are not normalized.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="65" href="https://cds.cern.ch/record/1993893/files/figs_twopt_tq_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_twopt_tq_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="66" href="https://cds.cern.ch/record/1993893/files/figs_twopt_qq_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_twopt_qq_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="67" href="https://cds.cern.ch/record/1993893/files/figs_twopt_qu_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_twopt_qu_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="68" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_ttq_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_ttq_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="69" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_tqq_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_tqq_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="70" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_qqu_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_qqu_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="71" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_uuu_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_uuu_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="72" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_ttq_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_ttq_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="73" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_tqq_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_tqq_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="74" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_qqu_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_qqu_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="75" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_uuu_dx11v2_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_uuu_dx11v2_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ \Planck\ 2015 CMB estimates and the corresponding means estimated from 1000 Monte Carlo simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equialteral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$ and $U_rU_rU_r$. The red solid, orange dot dot dot-dashed, green dashed and blue dot-dashed lines correspond to the \commander, \nilc, \sevem, and \smica\ maps, respectively. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="76" href="https://cds.cern.ch/record/1993893/files/figs_Fig7_new_compsep_robustness_test_88mm.png"><img src="https://cds.cern.ch/record/1993893/files/figs_Fig7_new_compsep_robustness_test_88mm.png" width="95%"/></a></td><td width="33%"> Lensing-induced $B$-mode power spectra in the component-separated polarization CMB maps. The solid line represents the best fit cosmology from the \Planck\ data release in 2015. Error bars were evaluated using a semi-analytical approximation validated over the FFP8 simulations as described in \citet{planck2014-pip116}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="77" href="https://cds.cern.ch/record/1993893/files/figs_commander_cmb_masks.png"><img src="https://cds.cern.ch/record/1993893/files/figs_commander_cmb_masks.png" width="95%"/></a></td><td width="33%"> \commander\ processing masks for temperature (\emph{top}) and polarization (\emph{bottom}). For temperature, the different shades of grey correspond to different angular resolutions, ranging from $5\arcm$ (light grey) through $7.5\arcm$ (dark grey) to 40\arcm\ FWHM (black). For polarization, the same mask is used for both 10\arcm\ and 40\arcm\ FWHM resolution.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="78" href="https://cds.cern.ch/record/1993893/files/figs_commander_cmb_masks_pol.png"><img src="https://cds.cern.ch/record/1993893/files/figs_commander_cmb_masks_pol.png" width="95%"/></a></td><td width="33%"> \commander\ processing masks for temperature (\emph{top}) and polarization (\emph{bottom}). For temperature, the different shades of grey correspond to different angular resolutions, ranging from $5\arcm$ (light grey) through $7.5\arcm$ (dark grey) to 40\arcm\ FWHM (black). For polarization, the same mask is used for both 10\arcm\ and 40\arcm\ FWHM resolution.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="79" href="https://cds.cern.ch/record/1993893/files/figs_commander_hybrid_overview.png"><img src="https://cds.cern.ch/record/1993893/files/figs_commander_hybrid_overview.png" width="95%"/></a></td><td width="33%"> Multipole moment weights used for multi-resolution hybridization in the \commander\ CMB map, as described by Eq.~\ref{eq:comm_hybrid}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="80" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_l1.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_l1.png" width="95%"/></a></td><td width="33%"> $5\deg\times5\deg$ zoom-in of the multi-resolution contributions to the \commander\ hybrid CMB map from the $40\arcm$ (\emph{top left}), $7\parcm5$ (\emph{top right}) and $\approx</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="81" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_l2.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_l2.png" width="95%"/></a></td><td width="33%"> $5\deg\times5\deg$ zoom-in of the multi-resolution contributions to the \commander\ hybrid CMB map from the $40\arcm$ (\emph{top left}), $7\parcm5$ (\emph{top right}) and $\approx</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="82" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_l3.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_l3.png" width="95%"/></a></td><td width="33%"> $5\deg\times5\deg$ zoom-in of the multi-resolution contributions to the \commander\ hybrid CMB map from the $40\arcm$ (\emph{top left}), $7\parcm5$ (\emph{top right}) and $\approx</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="83" href="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_hybrid.png"><img src="https://cds.cern.ch/record/1993893/files/figs_comm_zoom_hybrid.png" width="95%"/></a></td><td width="33%"> $5\deg\times5\deg$ zoom-in of the multi-resolution contributions to the \commander\ hybrid CMB map from the $40\arcm$ (\emph{top left}), $7\parcm5$ (\emph{top right}) and $\approx</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="84" href="https://cds.cern.ch/record/1993893/files/figs_needlet_bands-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_needlet_bands-crop.png" width="95%"/></a></td><td width="33%"> Needlet bands used in the analysis. The solid black line shows the normalization of the needlet bands, that is, the total filter applied to the original map after needlet decomposition and synthesis of the output map from needlet coefficients.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="85" href="https://cds.cern.ch/record/1993893/files/figs_iweight_mean_plot_xlog_ylin-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_iweight_mean_plot_xlog_ylin-crop.png" width="95%"/></a></td><td width="33%"> Full-sky average of needlet weights for different frequency channels and needlet bands. From top to bottom, the panels show results for temperature, $E$, and $B$ modes.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="86" href="https://cds.cern.ch/record/1993893/files/figs_eweight_mean_plot_xlog_ylin-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_eweight_mean_plot_xlog_ylin-crop.png" width="95%"/></a></td><td width="33%"> Full-sky average of needlet weights for different frequency channels and needlet bands. From top to bottom, the panels show results for temperature, $E$, and $B$ modes.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="87" href="https://cds.cern.ch/record/1993893/files/figs_bweight_mean_plot_xlog_ylin-crop.png"><img src="https://cds.cern.ch/record/1993893/files/figs_bweight_mean_plot_xlog_ylin-crop.png" width="95%"/></a></td><td width="33%"> Full-sky average of needlet weights for different frequency channels and needlet bands. From top to bottom, the panels show results for temperature, $E$, and $B$ modes.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="88" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_int_mask_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_int_mask_005a_2048.png" width="95%"/></a></td><td width="33%"> \nilc\ masks for temperature (\emph{top}) and polarization (\emph{bottom}).</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="89" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_pol_mask_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_nilc_pol_mask_005a_2048.png" width="95%"/></a></td><td width="33%"> \nilc\ masks for temperature (\emph{top}) and polarization (\emph{bottom}).</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="90" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_int_mask_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_int_mask_005a_2048.png" width="95%"/></a></td><td width="33%"> \sevem\ masks in temperature (\emph{top}) and polarization (\emph{bottom}).</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="91" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_pol_mask_010a_1024.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_sevem_pol_mask_010a_1024.png" width="95%"/></a></td><td width="33%"> \sevem\ masks in temperature (\emph{top}) and polarization (\emph{bottom}).</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="92" href="https://cds.cern.ch/record/1993893/files/figs_smica_filter_dx11.png"><img src="https://cds.cern.ch/record/1993893/files/figs_smica_filter_dx11.png" width="95%"/></a></td><td width="33%"> \smica\ weights for temperature (\emph{top}) and polarization (\emph{bottom}). For readibility, the values are shown for input maps in units of antenna temperature. The plot goes up to $\ell\sim3600$, but the output maps are synthesized uses all multipoles up to $\ell=4000$. For polarization, the thick solid lines show the contribution of input $E$ modes to the CMB $E$ modes and the thick dashed lines show the same for the $B$ modes. The thin lines, all close to zero, show ``cross-contributions'' of input $E$ modes to the CMB $B$ modes and vice versa.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="93" href="https://cds.cern.ch/record/1993893/files/figs_smica_filterEB_dx11.png"><img src="https://cds.cern.ch/record/1993893/files/figs_smica_filterEB_dx11.png" width="95%"/></a></td><td width="33%"> \smica\ weights for temperature (\emph{top}) and polarization (\emph{bottom}). For readibility, the values are shown for input maps in units of antenna temperature. The plot goes up to $\ell\sim3600$, but the output maps are synthesized uses all multipoles up to $\ell=4000$. For polarization, the thick solid lines show the contribution of input $E$ modes to the CMB $E$ modes and the thick dashed lines show the same for the $B$ modes. The thin lines, all close to zero, show ``cross-contributions'' of input $E$ modes to the CMB $B$ modes and vice versa.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="94" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_int_mask_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_int_mask_005a_2048.png" width="95%"/></a></td><td width="33%"> \smica\ masks in temperature (\emph{top}) and polarization (\emph{bottom}).</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="95" href="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_pol_mask_005a_2048.png"><img src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_smica_pol_mask_005a_2048.png" width="95%"/></a></td><td width="33%"> \smica\ masks in temperature (\emph{top}) and polarization (\emph{bottom}).</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="96" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_commander_nilc_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_commander_nilc_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between CMB temperature maps obtained on FFP8 simulations. Prior to differencing, the maps have been smoothed to 80 arcminutes FWHM and downgraded to N$_{side}$ = 128.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="97" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_commander_sevem_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_commander_sevem_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between CMB temperature maps obtained on FFP8 simulations. Prior to differencing, the maps have been smoothed to 80 arcminutes FWHM and downgraded to N$_{side}$ = 128.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="98" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_commander_smica_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_commander_smica_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between CMB temperature maps obtained on FFP8 simulations. Prior to differencing, the maps have been smoothed to 80 arcminutes FWHM and downgraded to N$_{side}$ = 128.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="99" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_nilc_sevem_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_nilc_sevem_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between CMB temperature maps obtained on FFP8 simulations. Prior to differencing, the maps have been smoothed to 80 arcminutes FWHM and downgraded to N$_{side}$ = 128.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="100" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_nilc_smica_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_nilc_smica_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between CMB temperature maps obtained on FFP8 simulations. Prior to differencing, the maps have been smoothed to 80 arcminutes FWHM and downgraded to N$_{side}$ = 128.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="101" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_sevem_smica_cmb_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_int_sevem_smica_cmb_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between CMB temperature maps obtained on FFP8 simulations. Prior to differencing, the maps have been smoothed to 80 arcminutes FWHM and downgraded to N$_{side}$ = 128.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="102" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_commander_nilc_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_commander_nilc_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $Q$ maps obtained on FFP8 siulations. Smoothing and degrading as in Fig.~\ref{fig:dx11_diff_I}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="103" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_commander_sevem_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_commander_sevem_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $Q$ maps obtained on FFP8 siulations. Smoothing and degrading as in Fig.~\ref{fig:dx11_diff_I}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="104" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_commander_smica_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_commander_smica_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $Q$ maps obtained on FFP8 siulations. Smoothing and degrading as in Fig.~\ref{fig:dx11_diff_I}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="105" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_nilc_sevem_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_nilc_sevem_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $Q$ maps obtained on FFP8 siulations. Smoothing and degrading as in Fig.~\ref{fig:dx11_diff_I}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="106" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_nilc_smica_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_nilc_smica_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $Q$ maps obtained on FFP8 siulations. Smoothing and degrading as in Fig.~\ref{fig:dx11_diff_I}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="107" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_sevem_smica_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_Q_sevem_smica_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $Q$ maps obtained on FFP8 siulations. Smoothing and degrading as in Fig.~\ref{fig:dx11_diff_I}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="108" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_commander_nilc_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_commander_nilc_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $U$ maps obtained on FFP8 siulations. Smoothing and degrading as in Figs.~\ref{fig:dx11_diff_I},\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="109" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_commander_sevem_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_commander_sevem_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $U$ maps obtained on FFP8 siulations. Smoothing and degrading as in Figs.~\ref{fig:dx11_diff_I},\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="110" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_commander_smica_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_commander_smica_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $U$ maps obtained on FFP8 siulations. Smoothing and degrading as in Figs.~\ref{fig:dx11_diff_I},\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="111" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_nilc_sevem_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_nilc_sevem_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $U$ maps obtained on FFP8 siulations. Smoothing and degrading as in Figs.~\ref{fig:dx11_diff_I},\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="112" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_nilc_smica_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_nilc_smica_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $U$ maps obtained on FFP8 siulations. Smoothing and degrading as in Figs.~\ref{fig:dx11_diff_I},\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="113" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_sevem_smica_cmb_hp_20_40_080a_0128.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_diff_U_sevem_smica_cmb_hp_20_40_080a_0128.png" width="95%"/></a></td><td width="33%"> Pairwise difference maps between $U$ maps obtained on FFP8 siulations. Smoothing and degrading as in Figs.~\ref{fig:dx11_diff_I},\ref{fig:dx11_diff_Q}.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="114" href="https://cds.cern.ch/record/1993893/files/figs_twopt_tt_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_twopt_tt_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions and the corresponding means estimated from 1000 MC simulations. From left to right, results for the 2-point, pseudo-collapsed 3-point, equilateral 3-point and connected rhombic 4-point functions for the $N_{\rm side}=64$ FFP8 CMB temperature estimates. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="115" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_ttt_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_ttt_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions and the corresponding means estimated from 1000 MC simulations. From left to right, results for the 2-point, pseudo-collapsed 3-point, equilateral 3-point and connected rhombic 4-point functions for the $N_{\rm side}=64$ FFP8 CMB temperature estimates. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="116" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_ttt_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_ttt_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions and the corresponding means estimated from 1000 MC simulations. From left to right, results for the 2-point, pseudo-collapsed 3-point, equilateral 3-point and connected rhombic 4-point functions for the $N_{\rm side}=64$ FFP8 CMB temperature estimates. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="117" href="https://cds.cern.ch/record/1993893/files/figs_fourpt_red_tttt_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_fourpt_red_tttt_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions and the corresponding means estimated from 1000 MC simulations. From left to right, results for the 2-point, pseudo-collapsed 3-point, equilateral 3-point and connected rhombic 4-point functions for the $N_{\rm side}=64$ FFP8 CMB temperature estimates. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="118" href="https://cds.cern.ch/record/1993893/files/figs_twopt_tq_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_twopt_tq_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="119" href="https://cds.cern.ch/record/1993893/files/figs_twopt_qq_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_twopt_qq_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="120" href="https://cds.cern.ch/record/1993893/files/figs_twopt_qu_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_twopt_qu_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="121" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_ttq_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_ttq_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="122" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_tqq_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_tqq_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="123" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_qqu_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_qqu_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="124" href="https://cds.cern.ch/record/1993893/files/figs_threept_coll_uuu_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_coll_uuu_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="125" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_ttq_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_ttq_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="126" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_tqq_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_tqq_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="127" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_qqu_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_qqu_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="128" href="https://cds.cern.ch/record/1993893/files/figs_threept_eq_uuu_ffp8_hp_diff_n64.png"><img src="https://cds.cern.ch/record/1993893/files/figs_threept_eq_uuu_ffp8_hp_diff_n64.png" width="95%"/></a></td><td width="33%"> The difference between the $N$-point functions for the high-pass filtered $N_{\rm side}=64$ FFP8 CMB estimates and the corresponding means estimated from 1000 MC simulations. The Stokes parameters $Q_r$ and $U_r$ were locally rotated so that the correlation functions are independent of coordinate frame. The first row shows results for the 2-point function, from left to right, $TQ_r$, $Q_rQ_r$, and $Q_rU_r$. The second row shows results for the pseudo-collapsed 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$, and the third row shows results for the equilateral 3-point function, from left to right, $TTQ_r$, $TQ_rQ_r$, $Q_rQ_rU_r$, and $U_rU_rU_r$. The black solid, red dot dot dot-dashed, orange dashed, green dot-dashed, and blue long dashed lines correspond to the true, {\tt Commander}, {\tt NILC}, {\tt SEVEM}, and {\tt SMICA} maps, respectively. The true CMB map was analysed with added noise corresponding to the {\tt SMICA} component separation method. The shaded dark and light grey regions indicate the 68\% and 95\% confidence regions, respectively, estimated using \smica\ simulations. See Sect.~\ref{sec:npoint_correlation} for the definition of the separation angle $\theta$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="129" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_spec_raw_TT.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_spec_raw_TT.png" width="95%"/></a></td><td width="33%"> Power spectra of the foreground cleaned CMB maps from FFP8 simulations. \emph{Top:} $TT$ power spectra evaluated using the \texttt{FFP8-UT74} mask. \emph{Bottom:} $EE$ power spectra evaluated using the \texttt{FFP8-UP76} mask. Thick lines show the spectra of signal plus noise estimated from the half-mission half-sum maps; thin lines show the noise levels from half-mission half-difference maps. The black line shows the input spectrum.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="130" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_spec_raw_EE.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_spec_raw_EE.png" width="95%"/></a></td><td width="33%"> Power spectra of the foreground cleaned CMB maps from FFP8 simulations. \emph{Top:} $TT$ power spectra evaluated using the \texttt{FFP8-UT74} mask. \emph{Bottom:} $EE$ power spectra evaluated using the \texttt{FFP8-UP76} mask. Thick lines show the spectra of signal plus noise estimated from the half-mission half-sum maps; thin lines show the noise levels from half-mission half-difference maps. The black line shows the input spectrum.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="131" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_int_components_paper_commander_preliminary.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_int_components_paper_commander_preliminary.png" width="95%"/></a></td><td width="33%"> $TT$ angular power spectra of residuals from the indicated FFP8 components in the \Planck\ 2015 CMB maps, compared with the predicted signal from the best fit cosmology. ``Other'' is the sum of CO, free-free, thermal and kinetic SZ, spinning dust, and synchrotron emission. The horizontal axis is linear in $\ell^{\,0.5}$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="132" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_int_components_paper_nilc_preliminary.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_int_components_paper_nilc_preliminary.png" width="95%"/></a></td><td width="33%"> $TT$ angular power spectra of residuals from the indicated FFP8 components in the \Planck\ 2015 CMB maps, compared with the predicted signal from the best fit cosmology. ``Other'' is the sum of CO, free-free, thermal and kinetic SZ, spinning dust, and synchrotron emission. The horizontal axis is linear in $\ell^{\,0.5}$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="133" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_int_components_paper_sevem_preliminary.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_int_components_paper_sevem_preliminary.png" width="95%"/></a></td><td width="33%"> $TT$ angular power spectra of residuals from the indicated FFP8 components in the \Planck\ 2015 CMB maps, compared with the predicted signal from the best fit cosmology. ``Other'' is the sum of CO, free-free, thermal and kinetic SZ, spinning dust, and synchrotron emission. The horizontal axis is linear in $\ell^{\,0.5}$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="134" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_int_components_paper_smica_preliminary.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_int_components_paper_smica_preliminary.png" width="95%"/></a></td><td width="33%"> $TT$ angular power spectra of residuals from the indicated FFP8 components in the \Planck\ 2015 CMB maps, compared with the predicted signal from the best fit cosmology. ``Other'' is the sum of CO, free-free, thermal and kinetic SZ, spinning dust, and synchrotron emission. The horizontal axis is linear in $\ell^{\,0.5}$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="135" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_pol_components_paper_commander_preliminary.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_pol_components_paper_commander_preliminary.png" width="95%"/></a></td><td width="33%"> $EE$ angular power spectra of residuals from the indicated FFP8 components in the \Planck\ 2015 CMB maps, compared with the predicted signal from the best fit cosmology. ``Other'' is the sum of CO, free-free, thermal and kinetic SZ, spinning dust, far-infrared background, and radio and infrared unresolved sources. The horizontal axis is linear in $\ell^{\,0.5}$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="136" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_pol_components_paper_nilc_preliminary.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_pol_components_paper_nilc_preliminary.png" width="95%"/></a></td><td width="33%"> $EE$ angular power spectra of residuals from the indicated FFP8 components in the \Planck\ 2015 CMB maps, compared with the predicted signal from the best fit cosmology. ``Other'' is the sum of CO, free-free, thermal and kinetic SZ, spinning dust, far-infrared background, and radio and infrared unresolved sources. The horizontal axis is linear in $\ell^{\,0.5}$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="137" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_pol_components_paper_sevem_preliminary.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_pol_components_paper_sevem_preliminary.png" width="95%"/></a></td><td width="33%"> $EE$ angular power spectra of residuals from the indicated FFP8 components in the \Planck\ 2015 CMB maps, compared with the predicted signal from the best fit cosmology. ``Other'' is the sum of CO, free-free, thermal and kinetic SZ, spinning dust, far-infrared background, and radio and infrared unresolved sources. The horizontal axis is linear in $\ell^{\,0.5}$.</td></tr></table><table width="95%" style="display: inline;"><tr><td width="66%"><a name="138" href="https://cds.cern.ch/record/1993893/files/figs_ffp8_pol_components_paper_smica_preliminary.png"><img src="https://cds.cern.ch/record/1993893/files/figs_ffp8_pol_components_paper_smica_preliminary.png" width="95%"/></a></td><td width="33%"> $EE$ angular power spectra of residuals from the indicated FFP8 components in the \Planck\ 2015 CMB maps, compared with the predicted signal from the best fit cosmology. ``Other'' is the sum of CO, free-free, thermal and kinetic SZ, spinning dust, far-infrared background, and radio and infrared unresolved sources. 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