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Planck 2015 results. IX. Diffuse component separation: CMB maps - CERN Document Server
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IX. 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" /> <!--[if lt IE 8]> <link href="https://cds.cern.ch/img/cern_toolbar/css/toolbar-ie.css" rel="stylesheet" type="text/css"> <![endif]--> <!--[if lt IE 8]> <link rel="stylesheet" type="text/css" href="https://cds.cern.ch/img/invenio-ie7.css" /> <![endif]--> <!--[if gt IE 8]> <style type="text/css">div.restrictedflag {filter:none;}</style> <![endif]--> <link rel="canonical" href="https://cds.cern.ch/record/1993893" /> <link rel="alternate" hreflang="el" href="https://cds.cern.ch/record/1993893?ln=el" /> <link rel="alternate" hreflang="fr" href="https://cds.cern.ch/record/1993893?ln=fr" /> <link rel="alternate" hreflang="bg" href="https://cds.cern.ch/record/1993893?ln=bg" /> <link rel="alternate" hreflang="zh-TW" href="https://cds.cern.ch/record/1993893?ln=zh_TW" /> <link rel="alternate" hreflang="pt" href="https://cds.cern.ch/record/1993893?ln=pt" /> <link rel="alternate" hreflang="no" href="https://cds.cern.ch/record/1993893?ln=no" /> <link rel="alternate" hreflang="hr" href="https://cds.cern.ch/record/1993893?ln=hr" /> <link rel="alternate" hreflang="ca" href="https://cds.cern.ch/record/1993893?ln=ca" /> <link rel="alternate" hreflang="de" href="https://cds.cern.ch/record/1993893?ln=de" /> <link rel="alternate" hreflang="it" href="https://cds.cern.ch/record/1993893?ln=it" /> <link rel="alternate" hreflang="zh-CN" href="https://cds.cern.ch/record/1993893?ln=zh_CN" /> <link rel="alternate" hreflang="sv" href="https://cds.cern.ch/record/1993893?ln=sv" /> <link rel="alternate" hreflang="sk" href="https://cds.cern.ch/record/1993893?ln=sk" /> <link rel="alternate" hreflang="en" href="https://cds.cern.ch/record/1993893?ln=en" /> <link rel="alternate" hreflang="pl" href="https://cds.cern.ch/record/1993893?ln=pl" /> <link rel="alternate" hreflang="ru" href="https://cds.cern.ch/record/1993893?ln=ru" /> <link rel="alternate" hreflang="ka" href="https://cds.cern.ch/record/1993893?ln=ka" /> <link rel="alternate" hreflang="ja" href="https://cds.cern.ch/record/1993893?ln=ja" /> <link rel="alternate" hreflang="es" href="https://cds.cern.ch/record/1993893?ln=es" /> <link rel="alternate" type="application/rss+xml" title="CERN Document Server RSS" href="/rss?ln=ru" /> <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="ru" /> <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> <!-- WebNews CSS library --> <link rel="stylesheet" href="https://cds.cern.ch/img/webnews.css" type="text/css" /> <!-- WebNews JS library --> <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> <!-- GoogleScholar --> <meta content="Planck 2015 results. 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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" /> <!-- Twitter Card --> <meta content="summary" name="twitter:card" /> <style></style> </head> <body class="CERN32Document32Server search" lang="ru"> <!-- toolbar starts --> <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=ru&referer=https%3A//cds.cern.ch/record/1993893%3Fln%3Dru" 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> <!-- toolbar ends --> <!-- Nav header starts--> <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><!-- /#name-and-slogan --> <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=ru">Искать</a></li> <li class="menu-444 "><a class="" title="" href="https://cds.cern.ch/submit?ln=ru">Внести</a></li> <li class="menu-426 "><a class="" href="https://cds.cern.ch/help/?ln=ru">Помощь</a></li> <li class="leaf hassubcdsmenu"> <a hreflang="en" class="header" href="https://cds.cern.ch/youraccount/display?ln=ru">Персонализовать</a> <ul class="subsubcdsmenu"><li><a href="https://cds.cern.ch/youralerts/list?ln=ru">Ваши оповещения</a></li><li><a href="https://cds.cern.ch/yourbaskets/display?ln=ru">Ваши книжные полки</a></li><li><a href="https://cds.cern.ch/yourcomments?ln=ru">Your comments</a></li><li><a href="https://cds.cern.ch/youralerts/display?ln=ru">Ваши поисковые запросы</a></li></ul></li> </ul> </div> </div> </div> <!-- Nav header ends--> <table class="navtrailbox"> <tr> <td class="navtrailboxbody"> <a href="/?ln=ru" class="navtrail">Главная страница</a> > Planck 2015 results. IX. Diffuse component separation: CMB maps </td> </tr> </table> </div> <div class="pagebody"><div class="pagebodystripemiddle"> <div class="detailedrecordbox"> <div class="detailedrecordtabs"> <div> <ul class="detailedrecordtabs"><li class="on first"><a href="/record/1993893/?ln=ru">Информация </a></li><li class=""><a href="/record/1993893/files?ln=ru">Файлы </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 style="height:0.1em;"> </div> <p class="notopgap"> </p>--> <abbr class="unapi-id" title="1993893"></abbr> <style type="text/css"> <!-- ul.detailedrecordtabs li.on a{background-color:#4D94CC;color:#fff !important;border-bottom:1px solid #4D94CC!important;} div.detailedrecordboxcontent {padding-top:0px !important;} --> </style> <table class="formatRecordTableFullWidth" > <tr> <td class="formatRecordHeader" style="background-image: url('https://cds.cern.ch/img/journals.jpg');" colspan="2"> <!--YTD: record may have more than one 690C.a tag--> Article </td> </tr> <script type="text/javascript"> $( document ).ready(function() { $('.showAuthor').on('click', function() { var author = '<p>' + $(this).data('name') + '</p>'; var affiliation = $(this).data('affiliation') + '</br>'; var contribution = $(this).data('contribution') + '</br>'; $.magnificPopup.open({ items: { src: '<div id="ovelary-mathjax" class="overlay-white oc-content overlay-white-500">' + author + affiliation + contribution + '</div>', type: 'inline' }, callbacks: { open: function() { var div = document.getElementById("overlay-mathjax") MathJax.Hub.Queue(["Typeset", MathJax.Hub, div]); }, } }) }) }); </script> <tr><td class="formatRecordLabel"> Report number </td><td style="padding-left:5px;"><a href="http://arxiv.org/abs/arXiv:1502.05956">arXiv:1502.05956</a></td></tr> <tr><td class="formatRecordLabel"> Title </td><td style="padding-left:5px;"><b>Planck 2015 results. IX. Diffuse component separation: CMB maps</b></td></tr> <tr><td class="formatRecordLabel"><span style="white-space:nowrap;"> Author(s) </span> </td><td style="padding-left:5px;"> <script type="text/javascript"> function toggle_authors_visibility(){ var more = document.getElementById('more'); var link = document.getElementById('link'); var extension = document.getElementById('extension'); if (more.style.display=='none'){ more.style.display = ''; extension.style.display = 'none'; link.innerHTML = "Руководство" } else { more.style.display = 'none'; extension.style.display = ''; link.innerHTML = "Показать всех 238 авторов" } link.style.color = "rgb(204,0,0);" } function set_up(){ var extension = document.getElementById('extension'); extension.innerHTML = "Planck Collaboration "; toggle_authors_visibility(); } </script> <a name="show_hide" /><p id="more" style=""><a href="https://cds.cern.ch/search?f=author&p=Adam%2C%20R.&ln=ru">Adam, R.</a> (LPSC, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Ade%2C%20P.A.R.&ln=ru">Ade, P.A.R.</a> (Cardiff U.) ; <a href="https://cds.cern.ch/search?f=author&p=Aghanim%2C%20N.&ln=ru">Aghanim, N.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Arnaud%2C%20M.&ln=ru">Arnaud, M.</a> (DAPNIA, Saclay) ; <a href="https://cds.cern.ch/search?f=author&p=Ashdown%2C%20M.&ln=ru">Ashdown, M.</a> (Cambridge U., KICC ; Cambridge U.) ; <a href="https://cds.cern.ch/search?f=author&p=Aumont%2C%20J.&ln=ru">Aumont, J.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Baccigalupi%2C%20C.&ln=ru">Baccigalupi, C.</a> (SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Banday%2C%20A.J.&ln=ru">Banday, A.J.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Barreiro%2C%20R.B.&ln=ru">Barreiro, R.B.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Bartlett%2C%20J.G.&ln=ru">Bartlett, J.G.</a> (APC, Paris ; Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Bartolo%2C%20N.&ln=ru">Bartolo, N.</a> (Padua U. ; INFN, Padua) ; <a href="https://cds.cern.ch/search?f=author&p=Basak%2C%20S.&ln=ru">Basak, S.</a> (SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Battaner%2C%20E.&ln=ru">Battaner, E.</a> (Granada U.) ; <a href="https://cds.cern.ch/search?f=author&p=Benabed%2C%20K.&ln=ru">Benabed, K.</a> (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <a href="https://cds.cern.ch/search?f=author&p=Benoit%2C%20A.&ln=ru">Benoit, A.</a> (Neel Lab, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Benoit-Levy%2C%20A.&ln=ru">Benoit-Levy, A.</a> (University Coll. London ; Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <a href="https://cds.cern.ch/search?f=author&p=Bernard%2C%20J.P.&ln=ru">Bernard, J.P.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Bersanelli%2C%20M.&ln=ru">Bersanelli, M.</a> (Milan U. ; Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Bielewicz%2C%20P.&ln=ru">Bielewicz, P.</a> (Toulouse III U. ; IRAP, Toulouse ; SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Bonaldi%2C%20A.&ln=ru">Bonaldi, A.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=Bonavera%2C%20L.&ln=ru">Bonavera, L.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Bond%2C%20J.R.&ln=ru">Bond, J.R.</a> (Canadian Inst. Theor. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Borrill%2C%20J.&ln=ru">Borrill, J.</a> (LBL, Berkeley ; UC, Berkeley) ; <a href="https://cds.cern.ch/search?f=author&p=Bouchet%2C%20F.R.&ln=ru">Bouchet, F.R.</a> (Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Boulanger%2C%20F.&ln=ru">Boulanger, F.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Bucher%2C%20M.&ln=ru">Bucher, M.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Burigana%2C%20C.&ln=ru">Burigana, C.</a> (Bologna Observ. ; Ferrara U. ; INFN, Bologna) ; <a href="https://cds.cern.ch/search?f=author&p=Butler%2C%20R.C.&ln=ru">Butler, R.C.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Calabrese%2C%20E.&ln=ru">Calabrese, E.</a> (Oxford U.) ; <a href="https://cds.cern.ch/search?f=author&p=Cardoso%2C%20J.F.&ln=ru">Cardoso, J.F.</a> (LTCI, Paris ; APC, Paris ; Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Casaponsa%2C%20B.&ln=ru">Casaponsa, B.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Castex%2C%20G.&ln=ru">Castex, G.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Catalano%2C%20A.&ln=ru">Catalano, A.</a> (LPSC, Grenoble ; LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Challinor%2C%20A.&ln=ru">Challinor, A.</a> (Cambridge U., Inst. of Astron. ; Cambridge U., KICC ; Cambridge U., DAMTP) ; <a href="https://cds.cern.ch/search?f=author&p=Chamballu%2C%20A.&ln=ru">Chamballu, A.</a> (DAPNIA, Saclay ; Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Chary%2C%20R.R.&ln=ru">Chary, R.R.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Chiang%2C%20H.C.&ln=ru">Chiang, H.C.</a> (Princeton U. ; KwaZulu Natal U.) ; <a href="https://cds.cern.ch/search?f=author&p=Christensen%2C%20P.R.&ln=ru">Christensen, P.R.</a> (Bohr Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Clements%2C%20D.L.&ln=ru">Clements, D.L.</a> (Imperial Coll., London) ; <a href="https://cds.cern.ch/search?f=author&p=Colombi%2C%20S.&ln=ru">Colombi, S.</a> (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <a href="https://cds.cern.ch/search?f=author&p=Colombo%2C%20L.P.L.&ln=ru">Colombo, L.P.L.</a> (UCLA ; Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Combet%2C%20C.&ln=ru">Combet, C.</a> (LPSC, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Couchot%2C%20F.&ln=ru">Couchot, F.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Coulais%2C%20A.&ln=ru">Coulais, A.</a> (LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Crill%2C%20B.P.&ln=ru">Crill, B.P.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Curto%2C%20A.&ln=ru">Curto, A.</a> (Cambridge U. ; Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Cuttaia%2C%20F.&ln=ru">Cuttaia, F.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Danese%2C%20L.&ln=ru">Danese, L.</a> (SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Davies%2C%20R.D.&ln=ru">Davies, R.D.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=Davis%2C%20R.J.&ln=ru">Davis, R.J.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=de%20Bernardis%2C%20P.&ln=ru">de Bernardis, P.</a> (Rome U.) ; <a href="https://cds.cern.ch/search?f=author&p=de%20Rosa%2C%20A.&ln=ru">de Rosa, A.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=de%20Zotti%2C%20G.&ln=ru">de Zotti, G.</a> (Padua Observ. ; SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Delabrouille%2C%20J.&ln=ru">Delabrouille, J.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Desert%2C%20F.X.&ln=ru">Desert, F.X.</a> (Grenoble Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Dickinson%2C%20C.&ln=ru">Dickinson, C.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=Diego%2C%20J.M.&ln=ru">Diego, J.M.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Dole%2C%20H.&ln=ru">Dole, H.</a> (Orsay ; IUF, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Donzelli%2C%20S.&ln=ru">Donzelli, S.</a> (Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Dore%2C%20O.&ln=ru">Dore, O.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Douspis%2C%20M.&ln=ru">Douspis, M.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Ducout%2C%20A.&ln=ru">Ducout, A.</a> (Paris, Inst. Astrophys. ; Imperial Coll., London) ; <a href="https://cds.cern.ch/search?f=author&p=Dupac%2C%20X.&ln=ru">Dupac, X.</a> (ESA, Madrid) ; <a href="https://cds.cern.ch/search?f=author&p=Efstathiou%2C%20G.&ln=ru">Efstathiou, G.</a> (Cambridge U., Inst. of Astron.) ; <a href="https://cds.cern.ch/search?f=author&p=Elsner%2C%20F.&ln=ru">Elsner, F.</a> (University Coll. London ; Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <a href="https://cds.cern.ch/search?f=author&p=Ensslin%2C%20T.A.&ln=ru">Ensslin, T.A.</a> (Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Eriksen%2C%20H.K.&ln=ru">Eriksen, H.K.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Falgarone%2C%20E.&ln=ru">Falgarone, E.</a> (LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Fantaye%2C%20Y.&ln=ru">Fantaye, Y.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Fergusson%2C%20J.&ln=ru">Fergusson, J.</a> (Cambridge U., DAMTP) ; <a href="https://cds.cern.ch/search?f=author&p=Finelli%2C%20F.&ln=ru">Finelli, F.</a> (Bologna Observ. ; INFN, Bologna) ; <a href="https://cds.cern.ch/search?f=author&p=Forni%2C%20O.&ln=ru">Forni, O.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Frailis%2C%20M.&ln=ru">Frailis, M.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Fraisse%2C%20A.A.&ln=ru">Fraisse, A.A.</a> (Princeton U.) ; <a href="https://cds.cern.ch/search?f=author&p=Franceschi%2C%20E.&ln=ru">Franceschi, E.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Frejsel%2C%20A.&ln=ru">Frejsel, A.</a> (Bohr Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Galeotta%2C%20S.&ln=ru">Galeotta, S.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Galli%2C%20S.&ln=ru">Galli, S.</a> (Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Ganga%2C%20K.&ln=ru">Ganga, K.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Ghosh%2C%20T.&ln=ru">Ghosh, T.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Giard%2C%20M.&ln=ru">Giard, M.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Giraud-Heraud%2C%20Y.&ln=ru">Giraud-Heraud, Y.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Gjerlow%2C%20E.&ln=ru">Gjerlow, E.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Gonzalez-Nuevo%2C%20J.&ln=ru">Gonzalez-Nuevo, J.</a> (Cantabria Inst. of Phys. ; SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Gorski%2C%20K.M.&ln=ru">Gorski, K.M.</a> (Caltech ; Warsaw U.) ; <a href="https://cds.cern.ch/search?f=author&p=Gratton%2C%20S.&ln=ru">Gratton, S.</a> (Cambridge U., KICC ; Cambridge U., Inst. of Astron.) ; <a href="https://cds.cern.ch/search?f=author&p=Gregorio%2C%20A.&ln=ru">Gregorio, A.</a> (Trieste U. ; Trieste Observ. ; INFN, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Gruppuso%2C%20A.&ln=ru">Gruppuso, A.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Gudmundsson%2C%20J.E.&ln=ru">Gudmundsson, J.E.</a> (Princeton U.) ; <a href="https://cds.cern.ch/search?f=author&p=Hansen%2C%20F.K.&ln=ru">Hansen, F.K.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Hanson%2C%20D.&ln=ru">Hanson, D.</a> (Rutherford ; Caltech ; Canadian Inst. Theor. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Harrison%2C%20D.L.&ln=ru">Harrison, D.L.</a> (Cambridge U., Inst. of Astron. ; Cambridge U., KICC) ; <a href="https://cds.cern.ch/search?f=author&p=Helou%2C%20G.&ln=ru">Helou, G.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Henrot-Versille%2C%20S.&ln=ru">Henrot-Versille, S.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Hernandez-Monteagudo%2C%20C.&ln=ru">Hernandez-Monteagudo, C.</a> (CEFCA, Teruel ; Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Herranz%2C%20D.&ln=ru">Herranz, D.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Hildebrandt%2C%20S.R.&ln=ru">Hildebrandt, S.R.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Hivon%2C%20E.&ln=ru">Hivon, E.</a> (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <a href="https://cds.cern.ch/search?f=author&p=Hobson%2C%20M.&ln=ru">Hobson, M.</a> (Cambridge U.) ; <a href="https://cds.cern.ch/search?f=author&p=Holmes%2C%20W.A.&ln=ru">Holmes, W.A.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Hornstrup%2C%20A.&ln=ru">Hornstrup, A.</a> (Denmark, Tech. U.) ; <a href="https://cds.cern.ch/search?f=author&p=Hovest%2C%20W.&ln=ru">Hovest, W.</a> (Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Huffenberger%2C%20K.M.&ln=ru">Huffenberger, K.M.</a> (Florida State U.) ; <a href="https://cds.cern.ch/search?f=author&p=Hurier%2C%20G.&ln=ru">Hurier, G.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Jaffe%2C%20A.H.&ln=ru">Jaffe, A.H.</a> (Imperial Coll., London) ; <a href="https://cds.cern.ch/search?f=author&p=Jaffe%2C%20T.R.&ln=ru">Jaffe, T.R.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Jones%2C%20W.C.&ln=ru">Jones, W.C.</a> (Princeton U.) ; <a href="https://cds.cern.ch/search?f=author&p=Juvela%2C%20M.&ln=ru">Juvela, M.</a> (Helsinki U.) ; <a href="https://cds.cern.ch/search?f=author&p=Keihanen%2C%20E.&ln=ru">Keihanen, E.</a> (Helsinki U.) ; <a href="https://cds.cern.ch/search?f=author&p=Keskitalo%2C%20R.&ln=ru">Keskitalo, R.</a> (LBL, Berkeley) ; <a href="https://cds.cern.ch/search?f=author&p=Kisner%2C%20T.S.&ln=ru">Kisner, T.S.</a> (LBL, Berkeley) ; <a href="https://cds.cern.ch/search?f=author&p=Kneissl%2C%20R.&ln=ru">Kneissl, R.</a> (European Southern Obs., Chile) ; <a href="https://cds.cern.ch/search?f=author&p=Knoche%2C%20J.&ln=ru">Knoche, J.</a> (Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Krachmalnicoff%2C%20N.&ln=ru">Krachmalnicoff, N.</a> (Milan U.) ; <a href="https://cds.cern.ch/search?f=author&p=Kunz%2C%20M.&ln=ru">Kunz, M.</a> (Geneva U. ; Orsay ; African Inst. Math. Sci., Cape Town) ; <a href="https://cds.cern.ch/search?f=author&p=Kurki-Suonio%2C%20H.&ln=ru">Kurki-Suonio, H.</a> (Helsinki U. ; Helsinki Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Lagache%2C%20G.&ln=ru">Lagache, G.</a> (Marseille, Lab. Astrophys. ; Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Lamarre%2C%20J.M.&ln=ru">Lamarre, J.M.</a> (LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Lasenby%2C%20A.&ln=ru">Lasenby, A.</a> (Cambridge U. ; Cambridge U., KICC) ; <a href="https://cds.cern.ch/search?f=author&p=Lattanzi%2C%20M.&ln=ru">Lattanzi, M.</a> (Ferrara U.) ; <a href="https://cds.cern.ch/search?f=author&p=Lawrence%2C%20C.R.&ln=ru">Lawrence, C.R.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Le%20Jeune%2C%20M.&ln=ru">Le Jeune, M.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Leonardi%2C%20R.&ln=ru">Leonardi, R.</a> (ESA, Madrid) ; <a href="https://cds.cern.ch/search?f=author&p=Lesgourgues%2C%20J.&ln=ru">Lesgourgues, J.</a> (CERN ; LPHE, Lausanne ; Savoie U.) ; <a href="https://cds.cern.ch/search?f=author&p=Levrier%2C%20F.&ln=ru">Levrier, F.</a> (LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Liguori%2C%20M.&ln=ru">Liguori, M.</a> (Padua U. ; INFN, Padua) ; <a href="https://cds.cern.ch/search?f=author&p=Lilje%2C%20P.B.&ln=ru">Lilje, P.B.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Linden-Vornle%2C%20M.&ln=ru">Linden-Vornle, M.</a> (Denmark, Tech. U.) ; <a href="https://cds.cern.ch/search?f=author&p=Lopez-Caniego%2C%20M.&ln=ru">Lopez-Caniego, M.</a> (ESA, Madrid ; Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Lubin%2C%20P.M.&ln=ru">Lubin, P.M.</a> (UC, Santa Barbara) ; <a href="https://cds.cern.ch/search?f=author&p=Macias-Perez%2C%20J.F.&ln=ru">Macias-Perez, J.F.</a> (LPSC, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Maggio%2C%20G.&ln=ru">Maggio, G.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Maino%2C%20D.&ln=ru">Maino, D.</a> (Milan U. ; Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Mandolesi%2C%20N.&ln=ru">Mandolesi, N.</a> (Bologna Observ. ; Ferrara U.) ; <a href="https://cds.cern.ch/search?f=author&p=Mangilli%2C%20A.&ln=ru">Mangilli, A.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Marshall%2C%20D.J.&ln=ru">Marshall, D.J.</a> (DAPNIA, Saclay) ; <a href="https://cds.cern.ch/search?f=author&p=Martin%2C%20P.G.&ln=ru">Martin, P.G.</a> (Canadian Inst. Theor. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Martinez-Gonzalez%2C%20E.&ln=ru">Martinez-Gonzalez, E.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Masi%2C%20S.&ln=ru">Masi, S.</a> (Rome U.) ; <a href="https://cds.cern.ch/search?f=author&p=Matarrese%2C%20S.&ln=ru">Matarrese, S.</a> (Padua U. ; INFN, Padua ; Gran Sasso) ; <a href="https://cds.cern.ch/search?f=author&p=Mazzotta%2C%20P.&ln=ru">Mazzotta, P.</a> (Rome U.) ; <a href="https://cds.cern.ch/search?f=author&p=McGehee%2C%20P.&ln=ru">McGehee, P.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Meinhold%2C%20P.R.&ln=ru">Meinhold, P.R.</a> (UC, Santa Barbara) ; <a href="https://cds.cern.ch/search?f=author&p=Melchiorri%2C%20A.&ln=ru">Melchiorri, A.</a> (Rome U. ; INFN, Rome) ; <a href="https://cds.cern.ch/search?f=author&p=Mendes%2C%20L.&ln=ru">Mendes, L.</a> (ESA, Madrid) ; <a href="https://cds.cern.ch/search?f=author&p=Mennella%2C%20A.&ln=ru">Mennella, A.</a> (Milan U. ; Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Migliaccio%2C%20M.&ln=ru">Migliaccio, M.</a> (Cambridge U., Inst. of Astron. ; Cambridge U., KICC) ; <a href="https://cds.cern.ch/search?f=author&p=Mitra%2C%20S.&ln=ru">Mitra, S.</a> (Pune U. ; Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Miville-Deschenes%2C%20M.A.&ln=ru">Miville-Deschenes, M.A.</a> (Orsay ; Canadian Inst. Theor. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Molinari%2C%20D.&ln=ru">Molinari, D.</a> (Cantabria Inst. of Phys. ; Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Moneti%2C%20A.&ln=ru">Moneti, A.</a> (Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Montier%2C%20L.&ln=ru">Montier, L.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Morgante%2C%20G.&ln=ru">Morgante, G.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Mortlock%2C%20D.&ln=ru">Mortlock, D.</a> (Imperial Coll., London) ; <a href="https://cds.cern.ch/search?f=author&p=Moss%2C%20A.&ln=ru">Moss, A.</a> (Nottingham U.) ; <a href="https://cds.cern.ch/search?f=author&p=Munshi%2C%20D.&ln=ru">Munshi, D.</a> (Cardiff U.) ; <a href="https://cds.cern.ch/search?f=author&p=Murphy%2C%20J.A.&ln=ru">Murphy, J.A.</a> (NUIM, Maynooth) ; <a href="https://cds.cern.ch/search?f=author&p=Naselsky%2C%20P.&ln=ru">Naselsky, P.</a> (Bohr Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Nati%2C%20F.&ln=ru">Nati, F.</a> (Princeton U.) ; <a href="https://cds.cern.ch/search?f=author&p=Natoli%2C%20P.&ln=ru">Natoli, P.</a> (Ferrara U. ; INFN, Rome2 ; Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Netterfield%2C%20C.B.&ln=ru">Netterfield, C.B.</a> (Toronto U.) ; <a href="https://cds.cern.ch/search?f=author&p=Norgaard-Nielsen%2C%20H.U.&ln=ru">Norgaard-Nielsen, H.U.</a> (Denmark, Tech. 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Astrophys. ; Paris U., VI-VII ; Illinois U., Urbana) ; <a href="https://cds.cern.ch/search?f=author&p=Wehus%2C%20I.K.&ln=ru">Wehus, I.K.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Yvon%2C%20D.&ln=ru">Yvon, D.</a> (DAPNIA, Saclay) ; <a href="https://cds.cern.ch/search?f=author&p=Zacchei%2C%20A.&ln=ru">Zacchei, A.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Zonca%2C%20A.&ln=ru">Zonca, A.</a> (UC, Santa Barbara)</p> <span id="extension"></span> <small><i><a id="link" href="#" onclick="toggle_authors_visibility()" style="color:rgb(204,0,0);"></a></i></small><script type="text/javascript">set_up()</script></td></tr> <tr><td class="formatRecordLabel"> Publication </td><td style="padding-left:5px;">2016-09-20</td></tr> <tr><td class="formatRecordLabel"> Imprint </td><td style="padding-left:5px;">20 Feb 2015</td></tr> <tr><td class="formatRecordLabel"> Number of pages </td><td style="padding-left:5px;">42</td></tr> <tr><td class="formatRecordLabel"> Note </td><td style="padding-left:5px;">Comments: 42 pages, 36 figures. Submitted to A&A<br />42 pages, 36 figures. Submitted to A&A</td></tr> <tr><td class="formatRecordLabel"> In: </td><td style="padding-left:5px;"><a href="http://dx.doi.org/10.1051/0004-6361/201525936"><i>Astron. Astrophys.</i> 594 (2016) A9</a> </a></td></tr> <tr><td class="formatRecordLabel"> DOI </td><td style="padding-left:5px;"><a href="http://dx.doi.org/10.1051/0004-6361/201525936" title="DOI" target="_blank">10.1051/0004-6361/201525936</a> <tr><td class="formatRecordLabel"> Subject category </td><td style="padding-left:5px;">Astrophysics and Astronomy</td></tr> <tr><td class="formatRecordLabel"> Abstract </td><td style="padding-left:5px;">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.</td></tr> <tr><td class="formatRecordLabel"> Copyright/License </td><td style="padding-left:5px;"><a href="http://arxiv.org/licenses/nonexclusive-distrib/1.0/">arXiv nonexclusive-distrib. 1.0</a></td></tr> </table> <br /><div style="max-width:1024px;margin:auto"><div style="overflow-x:auto;display:inline;width:100%;"><a href="/record/1993893/plots#0"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_common_int_mask_005a_2048.png" title=" Preferred masks for analysing component-separated CMB maps in temperature (\emph{left}) and polarization (\emph{right})." width="200px"/></a> <a href="/record/1993893/plots#1"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_common_pol_mask_new_010a_1024.png" title=" Preferred masks for analysing component-separated CMB maps in temperature (\emph{left}) and polarization (\emph{right})." width="200px"/></a> <a href="/record/1993893/plots#2"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/1993893/files/figs_dx11_v2_commander_int_cmb_005a_2048.png" title=" Component-separated CMB temperature maps at full resolution, FWHM 5\arcm, $\nside = 2048$." width="200px"/></a> <a href='/record/1993893/plots'>Show more plots</a></div></div><br /> <br/>Corresponding record in: <a href="http://inspirehep.net/record/1345438">Inspire</a> <small> </small> <br/> <br/><br/><div align="right"><div style="padding-bottom:2px;padding-top:30px;"><span class="moreinfo" style="margin-right:10px;"> <a href="" class="moreinfo">Back to search</a> </span></div></div> <div class="bottom-left-folded"><div class="recordlastmodifiedbox" style="position:relative;margin-left:1px"> Запись создана 2015-02-24, последняя модификация 2024-05-03</div></div> <div class="bottom-right-folded" style="text-align:right;padding-bottom:2px;"> <span class="moreinfo" style="margin-right:10px;"><a href="/search?ln=ru&p=recid%3A1993893&rm=wrd" class="moreinfo">Подобные записи</a></span></div> </div> </div> </div> <br/> <br /> <div class="detailedrecordminipanel"> <div class="top-left"></div><div class="top-right"></div> <div class="inside"> <div id="detailedrecordminipanelfile" style="width:33%;float:left;text-align:center;margin-top:0"> <div><small class="detailedRecordActions">Полный текст:</small> <br /><a href="/record/1993893/files/arXiv:1502.05956.pdf"><img style="border:none" src="/img/file-icon-text-12x16.gif" alt="Загрузка полного текста"/>PDF</a><br /></div><small class="detailedRecordActions">%(x_sitename) ссылка:</small><br /><small><a href="http://arxiv.org/pdf/1502.05956.pdf"><img style="border:none" src="/img/file-icon-text-12x16.gif" alt="Загрузка полного текста"/>Preprint</a></small> </div> <div id="detailedrecordminipanelreview" style="width:30%;float:left;text-align:center"> </div> <div id="detailedrecordminipanelactions" style="width:36%;float:right;text-align:right;"> <ul class="detailedrecordactions"> <li><a href="/yourbaskets/add?ln=ru&recid=1993893">Добавить в личную книжную полку</a></li> <li>Экспортировать как <a style="text-decoration:underline;font-weight:normal" href="/record/1993893/export/hx?ln=ru">BibTeX</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1993893/export/hm?ln=ru">MARC</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1993893/export/xm?ln=ru">MARCXML</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1993893/export/xd?ln=ru">DC</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1993893/export/xe?ln=ru">EndNote</a>, <!-- <a style="text-decoration:underline;font-weight:normal" href="/record/1993893/export/xe8x?ln=ru">EndNote (8-X)</a>,--> <a style="text-decoration:underline;font-weight:normal" href="/record/1993893/export/xn?ln=ru">NLM</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1993893/export/xw?ln=ru">RefWorks</a> </li> </ul> <div style='padding-left: 13px;'> <!-- JQuery Bookmark Button BEGIN --> <div id="bookmark"></div> <div id="bookmark_sciencewise"></div> <style type="text/css"> #bookmark_sciencewise, #bookmark {float: left;} #bookmark_sciencewise li {padding: 2px; 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IX. Diffuse component separation: CMB maps", description: "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. 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