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CMB power spectra, likelihoods, and robustness of parameters - 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/2033384" /> <link rel="alternate" hreflang="el" href="https://cds.cern.ch/record/2033384?ln=el" /> <link rel="alternate" hreflang="fr" href="https://cds.cern.ch/record/2033384?ln=fr" /> <link rel="alternate" hreflang="bg" href="https://cds.cern.ch/record/2033384?ln=bg" /> <link rel="alternate" hreflang="zh-TW" href="https://cds.cern.ch/record/2033384?ln=zh_TW" /> <link rel="alternate" hreflang="pt" href="https://cds.cern.ch/record/2033384?ln=pt" /> <link rel="alternate" hreflang="no" href="https://cds.cern.ch/record/2033384?ln=no" /> <link rel="alternate" hreflang="hr" href="https://cds.cern.ch/record/2033384?ln=hr" /> <link rel="alternate" hreflang="ca" href="https://cds.cern.ch/record/2033384?ln=ca" /> <link rel="alternate" hreflang="de" href="https://cds.cern.ch/record/2033384?ln=de" /> <link rel="alternate" hreflang="it" href="https://cds.cern.ch/record/2033384?ln=it" /> <link rel="alternate" hreflang="zh-CN" href="https://cds.cern.ch/record/2033384?ln=zh_CN" /> <link rel="alternate" hreflang="sv" href="https://cds.cern.ch/record/2033384?ln=sv" /> <link rel="alternate" hreflang="sk" href="https://cds.cern.ch/record/2033384?ln=sk" /> <link rel="alternate" hreflang="en" href="https://cds.cern.ch/record/2033384?ln=en" /> <link rel="alternate" hreflang="pl" href="https://cds.cern.ch/record/2033384?ln=pl" /> <link rel="alternate" hreflang="ru" href="https://cds.cern.ch/record/2033384?ln=ru" /> <link rel="alternate" hreflang="ka" href="https://cds.cern.ch/record/2033384?ln=ka" /> <link rel="alternate" hreflang="ja" href="https://cds.cern.ch/record/2033384?ln=ja" /> <link rel="alternate" hreflang="es" href="https://cds.cern.ch/record/2033384?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="This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlation functions of CMB temperature and polarization. They use the hybrid approach employed previously: pixel-based at low multipoles, $\ell$, and a Gaussian approximation to the distribution of cross-power spectra at higher $\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models. More than doubling the data allows further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction, contributing to enhanced precision. Improvements in processing and instrumental models further reduce uncertainties. Extensive tests establish robustness and accuracy, from temperature, from polarization, and from their combination, and show that the {\Lambda}CDM model continues to offer a very good fit. We further validate the likelihood against specific extensions to this baseline, such as the effective number of neutrino species. For this first detailed analysis of Planck polarization, we concentrate at high $\ell$ on E modes. At low $\ell$ we use temperature at all Planck frequencies along with a subset of polarization. These data take advantage of Planck's wide frequency range to improve the separation of CMB and foregrounds. Within the baseline cosmology this requires a reionization optical depth $\tau=0.078\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\ell$ we detect residual errors in E, typically at the {\mu}K$^2$ level; we thus recommend temperature alone as the high-$\ell$ baseline. Nevertheless, Planck high-$\ell$ polarization spectra are already good enough to allow a separate high-accuracy determination of the {\Lambda}CDM parameters, consistent with those established from temperature alone. This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlationfunctions of the cosmic microwave background (CMB) temperature and polarization fluctuations that account for relevant uncertainties, both instrumental and astrophysical in nature. They are based on the same hybrid approach used for the previous release, i.e., a pixel-based likelihood at low multipoles (l) and a Gaussian approximation to the distribution of cross-power spectra at higher multipoles. The main improvements are the use of more and better processed data and of Planck polarization information, along with more detailed models of foregrounds and instrumental uncertainties. The increased redundancy brought by more than doubling the amount of data analysed enables further consistency checks and enhanced immunity to systematic effects. It also improves the constraining power of Planck, in particular with regard to small-scale foreground properties. Progress in the modelling of foreground emission enables the retention of a larger fraction of the sky to determine the properties of the CMB, which also contributes to the enhanced precision of the spectra. Improvements in data processing and instrumental modelling further reduce uncertainties. Extensive tests establish the robustness and accuracy of the likelihood results, from temperature alone, from polarization alone, and from their combination. For temperature, we also perform a full likelihood analysis of realistic end-to-end simulations of the instrumental response to the sky, which were fed into the actual data processing pipeline; this does not reveal biases from residual low-level instrumental systematics. Even with the increase in precision and robustness, the LambdaCDM cosmological model continues to offer a very good fit to the Planck data. The slope of the primordial scalar fluctuations, n_s, is confirmed smaller than unity at more than 5sigma from Planck alone. We further validate the robustness of the likelihood results against specific extensions to the baseline cosmology, which are particularly sensitive to data at high multipoles. For instance, the effective number of neutrino species remains compatible with the canonical value of 3.046. For this first detailed analysis of Planck polarization spectra, we concentrate at high multipoles on the E modes, leaving the analysis of the weaker B modes to future work. At low multipoles we use temperature maps at all Planck frequencies along with a subset of polarization data. These data take advantage of Planck's wide frequency coverage to improve the separation of CMB and foreground emission. Within the baseline LambdaCDM cosmology this requires tau = 0.078 +- 0.019 for the reionization optical depth, which is significantly lower than estimates without the use of high-frequency data for explicit monitoring of dust emission. At high multipoles we detect residual systematic errors in E polarization, typically at the muK^2 level; we therefore choose to retain temperature information alone for high multipoles as the recommended baseline, in particular for testing non-minimal models. Nevertheless, the high-multipole polarization spectra from Planck are already good enough to enable a separate high-precision determination of the parameters of the LambdaCDM model, showing consistency with those established independently from temperature information alone. This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlations of CMB data, using the hybrid approach employed previously: pixel-based at $\ell<30$ and a Gaussian approximation to the distribution of spectra at higher $\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models, allowing further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction. Improvements in processing and instrumental models further reduce uncertainties. For temperature, we perform an analysis of end-to-end instrumental simulations fed into the data processing pipeline; this does not reveal biases from residual instrumental systematics. The $\Lambda$CDM cosmological model continues to offer a very good fit to Planck data. The slope of primordial scalar fluctuations, $n_s$, is confirmed smaller than unity at more than 5{\sigma} from Planck alone. We further validate robustness against specific extensions to the baseline cosmology. E.g., the effective number of neutrino species remains compatible with the canonical value of 3.046. This first detailed analysis of Planck polarization concentrates on E modes. At low $\ell$ we use temperature at all frequencies and a subset of polarization. The frequency range improves CMB-foreground separation. Within the baseline model this requires a reionization optical depth $\tau=0.078\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\ell$ we detect residual errors in E, typically O($\mu$K$^2$); we recommend temperature alone as the high-$\ell$ baseline. Nevertheless, Planck high-$\ell$ polarization allows a separate determination of $\Lambda$CDM parameters consistent with those from temperature alone. Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A.J.; Barreiro, R.B.; Bartlett, J.G.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoit, A.; Benoit-Levy, A.; Bernard, J.P.; Bersanelli, M.; Bielewicz, P.; Bock, J.J.; 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.; Catalano, A.; Challinor, A.; Chiang, H.C.; Christensen, P.R.; Clements, D.L.; Colombo, L.P.L.; Combet, C.; 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.; Di Valentino, E.; Dickinson, C.; Diego, J.M.; Dolag, K.; Dole, H.; Donzelli, S.; Dore, O.; Douspis, M.; Ducout, A.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Elsner, F.; Ensslin, T.A.; Eriksen, H.K.; Fergusson, J.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A.A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Gauthier, C.; Gerbino, M.; Giard, M.; Gjerlow, E.; Gonzalez-Nuevo, J.; Gorski, K.M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J.E.; Hamann, J.; Hansen, F.K.; Harrison, D.L.; Helou, G.; Henrot-Versille, S.; Hernandez-Monteagudo, C.; Herranz, D.; Hildebrandt, S.R.; Hivon, E.; Holmes, W.A.; Hornstrup, A.; Huffenberger, K.M.; Hurier, G.; Jaffe, A.H.; Jones, W.C.; Juvela, M.; Keihanen, E.; Keskitalo, R.; Kiiveri, K.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lahteenmaki, A.; Lamarre, J.M.; Lasenby, A.; Lattanzi, M.; Lawrence, C.R.; Le Jeune, M.; Leonardi, R.; Lesgourgues, J.; Levrier, F.; Lewis, A.; Liguori, M.; Lilje, P.B.; Lilley, M.; Linden-Vornle, M.; Lindholm, V.; Lopez-Caniego, M.; Macias-Perez, J.F.; Maffei, B.; Maggio, G.; Maino, D.; Mandolesi, N.; Mangilli, A.; Maris, M.; Martin, P.G.; Martinez-Gonzalez, E.; Masi, S.; Matarrese, S.; Meinhold, P.R.; Melchiorri, A.; Migliaccio, M.; Millea, M.; Miville-Deschenes, M.A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J.A.; Narimani, A.; Naselsky, P.; Nati, F.; Natoli, P.; Noviello, F.; Novikov, D.; Novikov, I.; Oxborrow, C.A.; Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, T.J.; Perdereau, O.; Perotto, L.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Pratt, G.W.; Prunet, S.; Puget, J.L.; Rachen, J.P.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ristorcelli, I.; Rocha, G.; Rossetti, M.; Roudier, G.; d'Orfeuil, B.Rouille; Rubino-Martin, J.A.; Rusholme, B.; Salvati, L.; Sandri, M.; Santos, D.; Savelainen, M.; Savini, G.; Scott, D.; Serra, P.; Spencer, L.D.; Spinelli, M.; Stolyarov, V.; Stompor, 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.; Umana, G.; 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. 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content="https://cds.cern.ch/record/2033384/files/figures_high_ell_USpipe_mspec_plik_cleaning.png" /> <meta property="og:image:secure_url" content="https://cds.cern.ch/record/2033384/files/figures_high_ell_USpipe_mspec_plik_cleaning.png" /> <meta property="og:image" content="https://cds.cern.ch/record/2033384/files/figures_high_ell_plik_cov_sim.png" /> <meta property="og:image:secure_url" content="https://cds.cern.ch/record/2033384/files/figures_high_ell_plik_cov_sim.png" /> <meta property="og:image" content="https://cds.cern.ch/record/2033384/files/figures_high_ell_Simulations_TTEETE_galf_TE_A_100_217.png" /> <meta property="og:image:secure_url" content="https://cds.cern.ch/record/2033384/files/figures_high_ell_Simulations_TTEETE_galf_TE_A_100_217.png" /> <meta content="CERN Document Server" property="og:site_name" /> <meta content="This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlation functions of CMB temperature and polarization. They use the hybrid approach employed previously: pixel-based at low multipoles, $\ell$, and a Gaussian approximation to the distribution of cross-power spectra at higher $\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models. More than doubling the data allows further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction, contributing to enhanced precision. Improvements in processing and instrumental models further reduce uncertainties. Extensive tests establish robustness and accuracy, from temperature, from polarization, and from their combination, and show that the {\Lambda}CDM model continues to offer a very good fit. We further validate the likelihood against specific extensions to this baseline, such as the effective number of neutrino species. For this first detailed analysis of Planck polarization, we concentrate at high $\ell$ on E modes. At low $\ell$ we use temperature at all Planck frequencies along with a subset of polarization. These data take advantage of Planck's wide frequency range to improve the separation of CMB and foregrounds. Within the baseline cosmology this requires a reionization optical depth $\tau=0.078\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\ell$ we detect residual errors in E, typically at the {\mu}K$^2$ level; we thus recommend temperature alone as the high-$\ell$ baseline. Nevertheless, Planck high-$\ell$ polarization spectra are already good enough to allow a separate high-accuracy determination of the {\Lambda}CDM parameters, consistent with those established from temperature alone." property="og:description" /> <meta content="This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlations of CMB data, using the hybrid approach employed previously: pixel-based at $\ell&lt;30$ and a Gaussian approximation to the distribution of spectra at higher $\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models, allowing further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction. Improvements in processing and instrumental models further reduce uncertainties. For temperature, we perform an analysis of end-to-end instrumental simulations fed into the data processing pipeline; this does not reveal biases from residual instrumental systematics. The $\Lambda$CDM cosmological model continues to offer a very good fit to Planck data. The slope of primordial scalar fluctuations, $n_s$, is confirmed smaller than unity at more than 5{\sigma} from Planck alone. We further validate robustness against specific extensions to the baseline cosmology. E.g., the effective number of neutrino species remains compatible with the canonical value of 3.046. This first detailed analysis of Planck polarization concentrates on E modes. At low $\ell$ we use temperature at all frequencies and a subset of polarization. The frequency range improves CMB-foreground separation. Within the baseline model this requires a reionization optical depth $\tau=0.078\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\ell$ we detect residual errors in E, typically O($\mu$K$^2$); we recommend temperature alone as the high-$\ell$ baseline. Nevertheless, Planck high-$\ell$ polarization allows a separate determination of $\Lambda$CDM parameters consistent with those from temperature alone." property="og:description" /> <meta content="This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlationfunctions of the cosmic microwave background (CMB) temperature and polarization fluctuations that account for relevant uncertainties, both instrumental and astrophysical in nature. They are based on the same hybrid approach used for the previous release, i.e., a pixel-based likelihood at low multipoles (l) and a Gaussian approximation to the distribution of cross-power spectra at higher multipoles. The main improvements are the use of more and better processed data and of Planck polarization information, along with more detailed models of foregrounds and instrumental uncertainties. The increased redundancy brought by more than doubling the amount of data analysed enables further consistency checks and enhanced immunity to systematic effects. It also improves the constraining power of Planck, in particular with regard to small-scale foreground properties. Progress in the modelling of foreground emission enables the retention of a larger fraction of the sky to determine the properties of the CMB, which also contributes to the enhanced precision of the spectra. Improvements in data processing and instrumental modelling further reduce uncertainties. Extensive tests establish the robustness and accuracy of the likelihood results, from temperature alone, from polarization alone, and from their combination. For temperature, we also perform a full likelihood analysis of realistic end-to-end simulations of the instrumental response to the sky, which were fed into the actual data processing pipeline; this does not reveal biases from residual low-level instrumental systematics. Even with the increase in precision and robustness, the LambdaCDM cosmological model continues to offer a very good fit to the Planck data. The slope of the primordial scalar fluctuations, n_s, is confirmed smaller than unity at more than 5sigma from Planck alone. We further validate the robustness of the likelihood results against specific extensions to the baseline cosmology, which are particularly sensitive to data at high multipoles. For instance, the effective number of neutrino species remains compatible with the canonical value of 3.046. For this first detailed analysis of Planck polarization spectra, we concentrate at high multipoles on the E modes, leaving the analysis of the weaker B modes to future work. At low multipoles we use temperature maps at all Planck frequencies along with a subset of polarization data. These data take advantage of Planck's wide frequency coverage to improve the separation of CMB and foreground emission. Within the baseline LambdaCDM cosmology this requires tau = 0.078 +- 0.019 for the reionization optical depth, which is significantly lower than estimates without the use of high-frequency data for explicit monitoring of dust emission. At high multipoles we detect residual systematic errors in E polarization, typically at the muK^2 level; we therefore choose to retain temperature information alone for high multipoles as the recommended baseline, in particular for testing non-minimal models. Nevertheless, the high-multipole polarization spectra from Planck are already good enough to enable a separate high-precision determination of the parameters of the LambdaCDM model, showing consistency with those established independently from temperature information alone." property="og:description" /> <meta content="arXiv" 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/2033384%3Fln%3Den" 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> > Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters </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/2033384/?ln=en">Information </a></li><li class=""><a href="/record/2033384/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">  <abbr class="unapi-id" title="2033384"></abbr> <style type="text/css">  </style> <table class="formatRecordTableFullWidth" > <tr> <td class="formatRecordHeader" style="background-image: url('https://cds.cern.ch/img/journals.jpg');" colspan="2">  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:1507.02704">arXiv:1507.02704</a></td></tr> <tr><td class="formatRecordLabel"> Title </td><td style="padding-left:5px;"><b>Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters</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 = "Hide" } else { more.style.display = 'none'; extension.style.display = ''; link.innerHTML = "Show all 221 authors" } 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=Aghanim%2C%20N.&ln=en">Aghanim, N.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Arnaud%2C%20M.&ln=en">Arnaud, M.</a> (DAPNIA, Saclay) ; <a href="https://cds.cern.ch/search?f=author&p=Ashdown%2C%20M.&ln=en">Ashdown, M.</a> (Cambridge U., KICC ; Cambridge U.) ; <a href="https://cds.cern.ch/search?f=author&p=Aumont%2C%20J.&ln=en">Aumont, J.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Baccigalupi%2C%20C.&ln=en">Baccigalupi, C.</a> (SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Banday%2C%20A.J.&ln=en">Banday, A.J.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Barreiro%2C%20R.B.&ln=en">Barreiro, R.B.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Bartlett%2C%20J.G.&ln=en">Bartlett, J.G.</a> (APC, Paris ; Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Bartolo%2C%20N.&ln=en">Bartolo, N.</a> (Padua U. ; INFN, Padua) ; <a href="https://cds.cern.ch/search?f=author&p=Battaner%2C%20E.&ln=en">Battaner, E.</a> (Granada U.) ; <a href="https://cds.cern.ch/search?f=author&p=Benabed%2C%20K.&ln=en">Benabed, K.</a> (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <a href="https://cds.cern.ch/search?f=author&p=Benoit%2C%20A.&ln=en">Benoit, A.</a> (Neel Lab, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Benoit-Levy%2C%20A.&ln=en">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=en">Bernard, J.P.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Bersanelli%2C%20M.&ln=en">Bersanelli, M.</a> (Milan U. ; Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Bielewicz%2C%20P.&ln=en">Bielewicz, P.</a> (Warsaw, Copernicus Astron. Ctr. ; IRAP, Toulouse ; SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Bock%2C%20J.J.&ln=en">Bock, J.J.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Bonaldi%2C%20A.&ln=en">Bonaldi, A.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=Bonavera%2C%20L.&ln=en">Bonavera, L.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Bond%2C%20J.R.&ln=en">Bond, J.R.</a> (Canadian Inst. Theor. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Borrill%2C%20J.&ln=en">Borrill, J.</a> (LBL, Berkeley ; UC, Berkeley) ; <a href="https://cds.cern.ch/search?f=author&p=Bouchet%2C%20F.R.&ln=en">Bouchet, F.R.</a> (Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Boulanger%2C%20F.&ln=en">Boulanger, F.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Bucher%2C%20M.&ln=en">Bucher, M.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Burigana%2C%20C.&ln=en">Burigana, C.</a> (Bologna Observ. ; Ferrara U. ; INFN, Bologna) ; <a href="https://cds.cern.ch/search?f=author&p=Butler%2C%20R.C.&ln=en">Butler, R.C.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Calabrese%2C%20E.&ln=en">Calabrese, E.</a> (Oxford U.) ; <a href="https://cds.cern.ch/search?f=author&p=Cardoso%2C%20J.F.&ln=en">Cardoso, J.F.</a> (LTCI, Paris ; APC, Paris ; Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Catalano%2C%20A.&ln=en">Catalano, A.</a> (LPSC, Grenoble ; LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Challinor%2C%20A.&ln=en">Challinor, A.</a> (Cambridge U., Inst. of Astron. ; Cambridge U., KICC ; Cambridge U., DAMTP) ; <a href="https://cds.cern.ch/search?f=author&p=Chiang%2C%20H.C.&ln=en">Chiang, H.C.</a> (Princeton U. ; KwaZulu Natal U.) ; <a href="https://cds.cern.ch/search?f=author&p=Christensen%2C%20P.R.&ln=en">Christensen, P.R.</a> (Bohr Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Clements%2C%20D.L.&ln=en">Clements, D.L.</a> (Imperial Coll., London) ; <a href="https://cds.cern.ch/search?f=author&p=Colombo%2C%20L.P.L.&ln=en">Colombo, L.P.L.</a> (UCLA ; Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Combet%2C%20C.&ln=en">Combet, C.</a> (LPSC, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Coulais%2C%20A.&ln=en">Coulais, A.</a> (LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Crill%2C%20B.P.&ln=en">Crill, B.P.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Curto%2C%20A.&ln=en">Curto, A.</a> (Cantabria Inst. of Phys. ; Cambridge U. ; Cambridge U., KICC) ; <a href="https://cds.cern.ch/search?f=author&p=Cuttaia%2C%20F.&ln=en">Cuttaia, F.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Danese%2C%20L.&ln=en">Danese, L.</a> (SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Davies%2C%20R.D.&ln=en">Davies, R.D.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=Davis%2C%20R.J.&ln=en">Davis, R.J.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=de%20Bernardis%2C%20P.&ln=en">de Bernardis, P.</a> (Rome U.) ; <a href="https://cds.cern.ch/search?f=author&p=de%20Rosa%2C%20A.&ln=en">de Rosa, A.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=de%20Zotti%2C%20G.&ln=en">de Zotti, G.</a> (Padua Observ. ; SISSA, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Delabrouille%2C%20J.&ln=en">Delabrouille, J.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Desert%2C%20F.X.&ln=en">Desert, F.X.</a> (Grenoble Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Di%20Valentino%2C%20E.&ln=en">Di Valentino, E.</a> (Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Dickinson%2C%20C.&ln=en">Dickinson, C.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=Diego%2C%20J.M.&ln=en">Diego, J.M.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Dolag%2C%20K.&ln=en">Dolag, K.</a> (Munich U. ; Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Dole%2C%20H.&ln=en">Dole, H.</a> (Orsay ; IUF, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Donzelli%2C%20S.&ln=en">Donzelli, S.</a> (Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Dore%2C%20O.&ln=en">Dore, O.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Douspis%2C%20M.&ln=en">Douspis, M.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Ducout%2C%20A.&ln=en">Ducout, A.</a> (Paris, Inst. Astrophys. ; Imperial Coll., London) ; <a href="https://cds.cern.ch/search?f=author&p=Dunkley%2C%20J.&ln=en">Dunkley, J.</a> (Oxford U.) ; <a href="https://cds.cern.ch/search?f=author&p=Dupac%2C%20X.&ln=en">Dupac, X.</a> (ESA, Madrid) ; <a href="https://cds.cern.ch/search?f=author&p=Efstathiou%2C%20G.&ln=en">Efstathiou, G.</a> (Cambridge U., Inst. of Astron.) ; <a href="https://cds.cern.ch/search?f=author&p=Elsner%2C%20F.&ln=en">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=en">Ensslin, T.A.</a> (Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Eriksen%2C%20H.K.&ln=en">Eriksen, H.K.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Fergusson%2C%20J.&ln=en">Fergusson, J.</a> (Cambridge U., DAMTP) ; <a href="https://cds.cern.ch/search?f=author&p=Finelli%2C%20F.&ln=en">Finelli, F.</a> (Bologna Observ. ; INFN, Bologna) ; <a href="https://cds.cern.ch/search?f=author&p=Forni%2C%20O.&ln=en">Forni, O.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Frailis%2C%20M.&ln=en">Frailis, M.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Fraisse%2C%20A.A.&ln=en">Fraisse, A.A.</a> (Princeton U.) ; <a href="https://cds.cern.ch/search?f=author&p=Franceschi%2C%20E.&ln=en">Franceschi, E.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Frejsel%2C%20A.&ln=en">Frejsel, A.</a> (Bohr Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Galeotta%2C%20S.&ln=en">Galeotta, S.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Galli%2C%20S.&ln=en">Galli, S.</a> (Chicago U., KICP) ; <a href="https://cds.cern.ch/search?f=author&p=Ganga%2C%20K.&ln=en">Ganga, K.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Gauthier%2C%20C.&ln=en">Gauthier, C.</a> (APC, Paris ; Taiwan, Natl. Taiwan U.) ; <a href="https://cds.cern.ch/search?f=author&p=Gerbino%2C%20M.&ln=en">Gerbino, M.</a> (Rome U.) ; <a href="https://cds.cern.ch/search?f=author&p=Giard%2C%20M.&ln=en">Giard, M.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Gjerlow%2C%20E.&ln=en">Gjerlow, E.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Gonzalez-Nuevo%2C%20J.&ln=en">Gonzalez-Nuevo, J.</a> (Oviedo U. ; Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Gorski%2C%20K.M.&ln=en">Gorski, K.M.</a> (Caltech ; Warsaw U.) ; <a href="https://cds.cern.ch/search?f=author&p=Gratton%2C%20S.&ln=en">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=en">Gregorio, A.</a> (Trieste U. ; Trieste Observ. ; INFN, Trieste) ; <a href="https://cds.cern.ch/search?f=author&p=Gruppuso%2C%20A.&ln=en">Gruppuso, A.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Gudmundsson%2C%20J.E.&ln=en">Gudmundsson, J.E.</a> (Princeton U.) ; <a href="https://cds.cern.ch/search?f=author&p=Hamann%2C%20J.&ln=en">Hamann, J.</a> (CERN ; Sydney U.) ; <a href="https://cds.cern.ch/search?f=author&p=Hansen%2C%20F.K.&ln=en">Hansen, F.K.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Harrison%2C%20D.L.&ln=en">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=en">Helou, G.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Henrot-Versille%2C%20S.&ln=en">Henrot-Versille, S.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Hernandez-Monteagudo%2C%20C.&ln=en">Hernandez-Monteagudo, C.</a> (CEFCA, Teruel ; Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Herranz%2C%20D.&ln=en">Herranz, D.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Hildebrandt%2C%20S.R.&ln=en">Hildebrandt, S.R.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Hivon%2C%20E.&ln=en">Hivon, E.</a> (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <a href="https://cds.cern.ch/search?f=author&p=Holmes%2C%20W.A.&ln=en">Holmes, W.A.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Hornstrup%2C%20A.&ln=en">Hornstrup, A.</a> (Denmark, Tech. U.) ; <a href="https://cds.cern.ch/search?f=author&p=Huffenberger%2C%20K.M.&ln=en">Huffenberger, K.M.</a> (Florida State U.) ; <a href="https://cds.cern.ch/search?f=author&p=Hurier%2C%20G.&ln=en">Hurier, G.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Jaffe%2C%20A.H.&ln=en">Jaffe, A.H.</a> (Imperial Coll., London) ; <a href="https://cds.cern.ch/search?f=author&p=Jones%2C%20W.C.&ln=en">Jones, W.C.</a> (Princeton U.) ; <a href="https://cds.cern.ch/search?f=author&p=Juvela%2C%20M.&ln=en">Juvela, M.</a> (Helsinki U.) ; <a href="https://cds.cern.ch/search?f=author&p=Keihanen%2C%20E.&ln=en">Keihanen, E.</a> (Helsinki U.) ; <a href="https://cds.cern.ch/search?f=author&p=Keskitalo%2C%20R.&ln=en">Keskitalo, R.</a> (LBL, Berkeley) ; <a href="https://cds.cern.ch/search?f=author&p=Kiiveri%2C%20K.&ln=en">Kiiveri, K.</a> (Helsinki U. ; Helsinki Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Knoche%2C%20J.&ln=en">Knoche, J.</a> (Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Knox%2C%20L.&ln=en">Knox, L.</a> (UC, Davis) ; <a href="https://cds.cern.ch/search?f=author&p=Kunz%2C%20M.&ln=en">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=en">Kurki-Suonio, H.</a> (Helsinki U. ; Helsinki Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Lagache%2C%20G.&ln=en">Lagache, G.</a> (Marseille, Lab. Astrophys. ; Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Lahteenmaki%2C%20A.&ln=en">Lahteenmaki, A.</a> (Aalto U. ; Helsinki Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Lamarre%2C%20J.M.&ln=en">Lamarre, J.M.</a> (LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Lasenby%2C%20A.&ln=en">Lasenby, A.</a> (Cambridge U. ; Cambridge U., KICC) ; <a href="https://cds.cern.ch/search?f=author&p=Lattanzi%2C%20M.&ln=en">Lattanzi, M.</a> (Ferrara U.) ; <a href="https://cds.cern.ch/search?f=author&p=Lawrence%2C%20C.R.&ln=en">Lawrence, C.R.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Le%20Jeune%2C%20M.&ln=en">Le Jeune, M.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Leonardi%2C%20R.&ln=en">Leonardi, R.</a> (ESA, Madrid) ; <a href="https://cds.cern.ch/search?f=author&p=Lesgourgues%2C%20J.&ln=en">Lesgourgues, J.</a> (Aachen, Tech. Hochsch. ; CERN) ; <a href="https://cds.cern.ch/search?f=author&p=Levrier%2C%20F.&ln=en">Levrier, F.</a> (LERMA, Ivry) ; <a href="https://cds.cern.ch/search?f=author&p=Lewis%2C%20A.&ln=en">Lewis, A.</a> (Sussex U.) ; <a href="https://cds.cern.ch/search?f=author&p=Liguori%2C%20M.&ln=en">Liguori, M.</a> (Padua U. ; INFN, Padua) ; <a href="https://cds.cern.ch/search?f=author&p=Lilje%2C%20P.B.&ln=en">Lilje, P.B.</a> (Oslo U.) ; <a href="https://cds.cern.ch/search?f=author&p=Lilley%2C%20M.&ln=en">Lilley, M.</a> (Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Linden-Vornle%2C%20M.&ln=en">Linden-Vornle, M.</a> (Denmark, Tech. U.) ; <a href="https://cds.cern.ch/search?f=author&p=Lindholm%2C%20V.&ln=en">Lindholm, V.</a> (Helsinki U. ; Helsinki Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Lopez-Caniego%2C%20M.&ln=en">Lopez-Caniego, M.</a> (ESA, Madrid ; Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Macias-Perez%2C%20J.F.&ln=en">Macias-Perez, J.F.</a> (LPSC, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Maffei%2C%20B.&ln=en">Maffei, B.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=Maggio%2C%20G.&ln=en">Maggio, G.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Maino%2C%20D.&ln=en">Maino, D.</a> (Milan U. ; Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Mandolesi%2C%20N.&ln=en">Mandolesi, N.</a> (Bologna Observ. ; Ferrara U.) ; <a href="https://cds.cern.ch/search?f=author&p=Mangilli%2C%20A.&ln=en">Mangilli, A.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Maris%2C%20M.&ln=en">Maris, M.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Martin%2C%20P.G.&ln=en">Martin, P.G.</a> (Canadian Inst. Theor. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Martinez-Gonzalez%2C%20E.&ln=en">Martinez-Gonzalez, E.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Masi%2C%20S.&ln=en">Masi, S.</a> (Rome U.) ; <a href="https://cds.cern.ch/search?f=author&p=Matarrese%2C%20S.&ln=en">Matarrese, S.</a> (Padua U. ; INFN, Padua ; Gran Sasso) ; <a href="https://cds.cern.ch/search?f=author&p=Meinhold%2C%20P.R.&ln=en">Meinhold, P.R.</a> (UC, Santa Barbara) ; <a href="https://cds.cern.ch/search?f=author&p=Melchiorri%2C%20A.&ln=en">Melchiorri, A.</a> (Rome U. ; INFN, Rome) ; <a href="https://cds.cern.ch/search?f=author&p=Migliaccio%2C%20M.&ln=en">Migliaccio, M.</a> (Cambridge U., Inst. of Astron. ; Cambridge U., KICC) ; <a href="https://cds.cern.ch/search?f=author&p=Millea%2C%20M.&ln=en">Millea, M.</a> (UC, Davis) ; <a href="https://cds.cern.ch/search?f=author&p=Miville-Deschenes%2C%20M.A.&ln=en">Miville-Deschenes, M.A.</a> (Orsay ; Canadian Inst. Theor. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Moneti%2C%20A.&ln=en">Moneti, A.</a> (Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Montier%2C%20L.&ln=en">Montier, L.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Morgante%2C%20G.&ln=en">Morgante, G.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Mortlock%2C%20D.&ln=en">Mortlock, D.</a> (Imperial Coll., London) ; <a href="https://cds.cern.ch/search?f=author&p=Munshi%2C%20D.&ln=en">Munshi, D.</a> (Cardiff U.) ; <a href="https://cds.cern.ch/search?f=author&p=Murphy%2C%20J.A.&ln=en">Murphy, J.A.</a> (NUIM, Maynooth) ; <a href="https://cds.cern.ch/search?f=author&p=Narimani%2C%20A.&ln=en">Narimani, A.</a> (British Columbia U.) ; <a href="https://cds.cern.ch/search?f=author&p=Naselsky%2C%20P.&ln=en">Naselsky, P.</a> (Bohr Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Nati%2C%20F.&ln=en">Nati, F.</a> (Princeton U.) ; <a href="https://cds.cern.ch/search?f=author&p=Natoli%2C%20P.&ln=en">Natoli, P.</a> (Ferrara U. ; INFN, Rome2 ; Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Noviello%2C%20F.&ln=en">Noviello, F.</a> (Manchester U.) ; <a href="https://cds.cern.ch/search?f=author&p=Novikov%2C%20D.&ln=en">Novikov, D.</a> (Lebedev Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Novikov%2C%20I.&ln=en">Novikov, I.</a> (Bohr Inst. ; Lebedev Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Oxborrow%2C%20C.A.&ln=en">Oxborrow, C.A.</a> (Denmark, Tech. 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Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Valenziano%2C%20L.&ln=en">Valenziano, L.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Valiviita%2C%20J.&ln=en">Valiviita, J.</a> (Helsinki U. ; Helsinki Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Van%20Tent%2C%20B.&ln=en">Van Tent, B.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Vielva%2C%20P.&ln=en">Vielva, P.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Villa%2C%20F.&ln=en">Villa, F.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Wade%2C%20L.A.&ln=en">Wade, L.A.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Wandelt%2C%20B.D.&ln=en">Wandelt, B.D.</a> (Paris, Inst. Astrophys. ; Paris U., VI-VII ; Illinois U., Urbana) ; <a href="https://cds.cern.ch/search?f=author&p=Wehus%2C%20I.K.&ln=en">Wehus, I.K.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Yvon%2C%20D.&ln=en">Yvon, D.</a> (DAPNIA, Saclay) ; <a href="https://cds.cern.ch/search?f=author&p=Zacchei%2C%20A.&ln=en">Zacchei, A.</a> (Trieste Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Zonca%2C%20A.&ln=en">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;">09 Jul 2015</td></tr> <tr><td class="formatRecordLabel"> Number of pages </td><td style="padding-left:5px;">99</td></tr> <tr><td class="formatRecordLabel"> Note </td><td style="padding-left:5px;">This paper is associated with the 2015 Planck release (see <a href="http://www.cosmos.esa.int/web/planck/publications).">http://www.cosmos.esa.int/web/planck/publications).</a> Likelihood code & data available at <a href="http://www.cosmos.esa.int/web/planck/pla.">http://www.cosmos.esa.int/web/planck/pla.</a> Version accepted by A&A.; Substancially extended (104 pages) with analysis of end-to-simulations of systematics further confirming the results. Abstract abridged</td></tr> <tr><td class="formatRecordLabel"> In: </td><td style="padding-left:5px;"><a href="http://dx.doi.org/10.1051/0004-6361/201526926"><i>Astron. Astrophys.</i> 594 (2016) A11</a> </a></td></tr> <tr><td class="formatRecordLabel"> DOI </td><td style="padding-left:5px;"><a href="http://dx.doi.org/10.1051/0004-6361/201526926" title="DOI" target="_blank">10.1051/0004-6361/201526926</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;">This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlation functions of CMB temperature and polarization. They use the hybrid approach employed previously: pixel-based at low multipoles, $\ell$, and a Gaussian approximation to the distribution of cross-power spectra at higher $\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models. More than doubling the data allows further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction, contributing to enhanced precision. Improvements in processing and instrumental models further reduce uncertainties. Extensive tests establish robustness and accuracy, from temperature, from polarization, and from their combination, and show that the {\Lambda}CDM model continues to offer a very good fit. We further validate the likelihood against specific extensions to this baseline, such as the effective number of neutrino species. For this first detailed analysis of Planck polarization, we concentrate at high $\ell$ on E modes. At low $\ell$ we use temperature at all Planck frequencies along with a subset of polarization. These data take advantage of Planck's wide frequency range to improve the separation of CMB and foregrounds. Within the baseline cosmology this requires a reionization optical depth $\tau=0.078\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\ell$ we detect residual errors in E, typically at the {\mu}K$^2$ level; we thus recommend temperature alone as the high-$\ell$ baseline. Nevertheless, Planck high-$\ell$ polarization spectra are already good enough to allow a separate high-accuracy determination of the {\Lambda}CDM parameters, consistent with those established from temperature alone.</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/2033384/plots#0"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/2033384/files/figures_low_ell_commander_cmb_temp_extdata_n256_60arc_v1_cr.png" title=" \emph{Top}: \commander\ CMB temperature map derived from the \Planck\ 2015, 9-year \WMAP, and 408$\,$MHz Haslam et al.\ observations, as described in \citet{planck2014-a12}. The gray boundary indicates the 2015 likelihood temperature mask, covering a total of 7\,\% of the sky. The masked area has been filled with a constrained Gaussian realization. \emph{Middle}: difference between the 2015 and 2013 \commander\ temperature maps. The masked region indicates the 2013 likelihood mask, removing 13\,\% of the sky. \emph{Bottom}: comparison of the 2013 (gray) and 2015 (black) temperature likelihood masks." width="200px"/></a> <a href="/record/2033384/plots#1"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/2033384/files/figures_low_ell_commander_diff_masked.png" title=" \emph{Top}: \commander\ CMB temperature map derived from the \Planck\ 2015, 9-year \WMAP, and 408$\,$MHz Haslam et al.\ observations, as described in \citet{planck2014-a12}. The gray boundary indicates the 2015 likelihood temperature mask, covering a total of 7\,\% of the sky. The masked area has been filled with a constrained Gaussian realization. \emph{Middle}: difference between the 2015 and 2013 \commander\ temperature maps. The masked region indicates the 2013 likelihood mask, removing 13\,\% of the sky. \emph{Bottom}: comparison of the 2013 (gray) and 2015 (black) temperature likelihood masks." width="200px"/></a> <a href="/record/2033384/plots#2"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/2033384/files/figures_low_ell_commander_mask_sum.png" title=" \emph{Top}: \commander\ CMB temperature map derived from the \Planck\ 2015, 9-year \WMAP, and 408$\,$MHz Haslam et al.\ observations, as described in \citet{planck2014-a12}. The gray boundary indicates the 2015 likelihood temperature mask, covering a total of 7\,\% of the sky. The masked area has been filled with a constrained Gaussian realization. \emph{Middle}: difference between the 2015 and 2013 \commander\ temperature maps. The masked region indicates the 2013 likelihood mask, removing 13\,\% of the sky. \emph{Bottom}: comparison of the 2013 (gray) and 2015 (black) temperature likelihood masks." width="200px"/></a> <a href='/record/2033384/plots'>Show more plots</a></div></div><br /> <br/>Corresponding record in: <a href="http://inspirehep.net/record/1382312">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"> Record created 2015-07-13, last modified 2024-06-07</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=en&p=recid%3A2033384&rm=wrd" class="moreinfo">Similar records</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">Fulltext:</small> <br /><a href="/record/2033384/files/arXiv:1507.02704.pdf"><img style="border:none" src="/img/file-icon-text-12x16.gif" alt="Download fulltext"/>PDF</a><br /></div><small class="detailedRecordActions">External link:</small><br /><small><a href="http://arxiv.org/pdf/1507.02704.pdf"><img style="border:none" src="/img/file-icon-text-12x16.gif" alt="Download fulltext"/>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=en&recid=2033384">Add to personal basket</a></li> <li>Export as <a style="text-decoration:underline;font-weight:normal" href="/record/2033384/export/hx?ln=en">BibTeX</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/2033384/export/hm?ln=en">MARC</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/2033384/export/xm?ln=en">MARCXML</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/2033384/export/xd?ln=en">DC</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/2033384/export/xe?ln=en">EndNote</a>,  <a style="text-decoration:underline;font-weight:normal" href="/record/2033384/export/xn?ln=en">NLM</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/2033384/export/xw?ln=en">RefWorks</a> </li> </ul> <div style='padding-left: 13px;'>  <div id="bookmark"></div> <div id="bookmark_sciencewise"></div> <style type="text/css"> #bookmark_sciencewise, #bookmark {float: left;} #bookmark_sciencewise li {padding: 2px; width: 25px;} #bookmark_sciencewise ul, #bookmark ul {list-style-image: none;} </style> <script type="text/javascript" src="/js/jquery.bookmark.min.js"></script> <style type="text/css">@import "/css/jquery.bookmark.css";</style> <script type="text/javascript">// <![CDATA[ $.bookmark.addSite('sciencewise', 'ScienceWise.info', 'https://cds.cern.ch/img/sciencewise.png', 'en', 'bookmark', 'http://sciencewise.info/bookmarks/1507.0270/add'); $('#bookmark_sciencewise').bookmark({sites: ['sciencewise']}); $('#bookmark').bookmark({ sites: ['facebook', 'twitter', 'linkedin', 'google_plusone'], icons: '/img/bookmarks.png', url: 'https://cds.cern.ch/record/2033384', addEmail: true, title: "Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters", description: "This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlation functions of CMB temperature and polarization. They use the hybrid approach employed previously: pixel-based at low multipoles, $\\ell$, and a Gaussian approximation to the distribution of cross-power spectra at higher $\\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models. More than doubling the data allows further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction, contributing to enhanced precision. Improvements in processing and instrumental models further reduce uncertainties. Extensive tests establish robustness and accuracy, from temperature, from polarization, and from their combination, and show that the {\\Lambda}CDM model continues to offer a very good fit. We further validate the likelihood against specific extensions to this baseline, such as the effective number of neutrino species. For this first detailed analysis of Planck polarization, we concentrate at high $\\ell$ on E modes. At low $\\ell$ we use temperature at all Planck frequencies along with a subset of polarization. These data take advantage of Planck\'s wide frequency range to improve the separation of CMB and foregrounds. Within the baseline cosmology this requires a reionization optical depth $\\tau=0.078\\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\\ell$ we detect residual errors in E, typically at the {\\mu}K$^2$ level; we thus recommend temperature alone as the high-$\\ell$ baseline. Nevertheless, Planck high-$\\ell$ polarization spectra are already good enough to allow a separate high-accuracy determination of the {\\Lambda}CDM parameters, consistent with those established from temperature alone." }); // ]]> </script>  </div> </div> <div style="clear:both;margin-bottom: 0;"></div> </div> <div class="bottom-left"></div><div class="bottom-right"></div> </div> </div></div> <footer id="footer" class="pagefooter clearfix">  <div class="pagefooterstripeleft"> CERN Document Server :: <a class="footer" href="https://cds.cern.ch/?ln=en">Search</a> :: <a class="footer" href="https://cds.cern.ch/submit?ln=en">Submit</a> :: <a class="footer" href="https://cds.cern.ch/youraccount/display?ln=en">Personalize</a> :: <a class="footer" href="https://cds.cern.ch/help/?ln=en">Help</a> :: <a class="footer" href="https://cern.service-now.com/service-portal?id=privacy_policy&se=CDS-Service" target="_blank">Privacy Notice</a> <br /> Powered by <a class="footer" href="http://invenio-software.org/">Invenio</a> <br /> Maintained by <a class="footer" href="https://cern.service-now.com/service-portal?id=service_element&name=CDS-Service">CDS Service</a> - Need help? 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