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The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes - 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/1757020" /> <link rel="alternate" hreflang="el" href="https://cds.cern.ch/record/1757020?ln=el" /> <link rel="alternate" hreflang="fr" href="https://cds.cern.ch/record/1757020?ln=fr" /> <link rel="alternate" hreflang="bg" href="https://cds.cern.ch/record/1757020?ln=bg" /> <link rel="alternate" hreflang="zh-TW" href="https://cds.cern.ch/record/1757020?ln=zh_TW" /> <link rel="alternate" hreflang="pt" href="https://cds.cern.ch/record/1757020?ln=pt" /> <link rel="alternate" hreflang="no" href="https://cds.cern.ch/record/1757020?ln=no" /> <link rel="alternate" hreflang="hr" href="https://cds.cern.ch/record/1757020?ln=hr" /> <link rel="alternate" hreflang="ca" href="https://cds.cern.ch/record/1757020?ln=ca" /> <link rel="alternate" hreflang="de" href="https://cds.cern.ch/record/1757020?ln=de" /> <link rel="alternate" hreflang="it" href="https://cds.cern.ch/record/1757020?ln=it" /> <link rel="alternate" hreflang="zh-CN" href="https://cds.cern.ch/record/1757020?ln=zh_CN" /> <link rel="alternate" hreflang="sv" href="https://cds.cern.ch/record/1757020?ln=sv" /> <link rel="alternate" hreflang="sk" href="https://cds.cern.ch/record/1757020?ln=sk" /> <link rel="alternate" hreflang="en" href="https://cds.cern.ch/record/1757020?ln=en" /> <link rel="alternate" hreflang="pl" href="https://cds.cern.ch/record/1757020?ln=pl" /> <link rel="alternate" hreflang="ru" href="https://cds.cern.ch/record/1757020?ln=ru" /> <link rel="alternate" hreflang="ka" href="https://cds.cern.ch/record/1757020?ln=ka" /> <link rel="alternate" hreflang="ja" href="https://cds.cern.ch/record/1757020?ln=ja" /> <link rel="alternate" hreflang="es" href="https://cds.cern.ch/record/1757020?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="The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100GHz. We exploit the Planck HFI polarization data from 100 to 353GHz to measure the dust angular power spectra $C_\ell^{EE,BB}$ over the range $40<\ell<600$. These will bring new insights into interstellar dust physics and a precise determination of the level of contamination for CMB polarization experiments. We show that statistical properties of the emission can be characterized over large fractions of the sky using $C_\ell$. For the dust, they are well described by power laws in $\ell$ with exponents $\alpha^{EE,BB}=-2.42\pm0.02$. The amplitudes of the polarization $C_\ell$ vary with the average brightness in a way similar to the intensity ones. The dust polarization frequency dependence is consistent with modified blackbody emission with $\beta_d=1.59$ and $T_d=19.6$K. We find a systematic ratio between the amplitudes of the Galactic $B$- and $E$-modes of 0.5. We show that even in the faintest dust-emitting regions there are no "clean" windows where primordial CMB $B$-mode polarization could be measured without subtraction of dust emission. Finally, we investigate the level of dust polarization in the BICEP2 experiment field. Extrapolation of the Planck 353GHz data to 150GHz gives a dust power $\ell(\ell+1)C_\ell^{BB}/(2\pi)$ of $1.32\times10^{-2}\mu$K$_{CMB}^2$ over the $40<\ell<120$ range; the statistical uncertainty is $\pm0.29$ and there is an additional uncertainty (+0.28,-0.24) from the extrapolation, both in the same units. This is the same magnitude as reported by BICEP2 over this $\ell$ range, which highlights the need for assessment of the polarized dust signal. The present uncertainties will be reduced through an ongoing, joint analysis of the Planck and BICEP2 data sets. The polarized thermal emission from diffuse Galactic dust is the main foreground presentin measurements of the polarization of the cosmic microwave background (CMB) atfrequencies above 100GHz. In this paper we exploit the uniqueness of thePlanck HFI polarization data from 100 to 353GHz to measure thepolarized dust angular power spectra C_l^EE and C_l^BB over themultipole range 40 well away from the Galactic plane. These measurements will bringnew insights into interstellar dust physics and allow a precise determination of the levelof contamination for CMB polarization experiments. Despite the non-Gaussian andanisotropic nature of Galactic dust, we show that general statistical properties of theemission can be characterized accurately over large fractions of the sky using angularpower spectra. The polarization power spectra of the dust are well described by power lawsin multipole, C_l ∝l^alpha, with exponentsalpha^EE,BB = -2.42 +- 0.02.The amplitudes of the polarization power spectra vary with the average brightness in a waysimilar to the intensity power spectra. The frequency dependence of the dust polarizationspectra is consistent with modified blackbody emission with beta_d = 1.59 andT_d = 19.6K down to the lowest Planck HFI frequencies. We find asystematic difference between the amplitudes of the Galactic B- and E-modes, C_l^BB/C_l^EE =0.5. We verify that these general properties are preserved towards highGalactic latitudes with low dust column densities. We show that even in the faintestdust-emitting regions there are no 'clean' windows in the sky where primordial CMBB-modepolarization measurements could be made without subtraction of foreground emission.Finally, we investigate the level of dust polarization in the specific field recentlytargeted by the BICEP2 experiment. Extrapolation of the Planck 353GHzdata to 150GHz gives a dust power 𝒟_l^BB =l(l+1)C_l^BB/(2pi) of 1.32 x 10^-2muK_CMB^2 over the multipole rangeof the primordial recombination bump (40); the statistical uncertainty is+- 0.29 x 10^-2muK_CMB^2 and there is anadditional uncertainty (+0.28, -0.24) x10^-2muK_CMB^2 from the extrapolation.This level is the same magnitude as reported by BICEP2 over this l range, which highlightsthe need for assessment of the polarized dust signal even in the cleanest windows of thesky. The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100GHz. We exploit the Planck HFI polarization data from 100 to 353GHz to measure the dust angular power spectra $C_\ell^{EE,BB}$ over the range $40<\ell<600$ well away from the Galactic plane. These will bring new insights into interstellar dust physics and a precise determination of the level of contamination for CMB polarization experiments. We show that statistical properties of the emission can be characterized over large fractions of the sky using $C_\ell$. For the dust, they are well described by power laws in $\ell$ with exponents $\alpha^{EE,BB}=-2.42\pm0.02$. The amplitudes of the polarization $C_\ell$ vary with the average brightness in a way similar to the intensity ones. The dust polarization frequency dependence is consistent with modified blackbody emission with $\beta_d=1.59$ and $T_d=19.6$K. We find a systematic ratio between the amplitudes of the Galactic $B$- and $E$-modes of 0.5. We show that even in the faintest dust-emitting regions there are no "clean" windows where primordial CMB $B$-mode polarization could be measured without subtraction of dust emission. Finally, we investigate the level of dust polarization in the BICEP2 experiment field. Extrapolation of the Planck 353GHz data to 150GHz gives a dust power $\ell(\ell+1)C_\ell^{BB}/(2\pi)$ of $1.32\times10^{-2}\mu$K$_{CMB}^2$ over the $40<\ell<120$ range; the statistical uncertainty is $\pm0.29$ and there is an additional uncertainty (+0.28,-0.24) from the extrapolation, both in the same units. This is the same magnitude as reported by BICEP2 over this $\ell$ range, which highlights the need for assessment of the polarized dust signal even in the cleanest windows of the sky. Adam, R.; Ade, P.A.R.; Aghanim, N.; Arnaud, M.; Aumont, J.; Baccigalupi, C.; Banday, A.J.; Barreiro, R.B.; Bartlett, J.G.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoit-Levy, A.; Bernard, J.P.; Bersanelli, M.; Bielewicz, P.; Bonaldi, A.; Bonavera, L.; Bond, J.R.; Borrill, J.; Bouchet, F.R.; Boulanger, F.; Bracco, A.; Bucher, M.; Burigana, C.; Butler, R.C.; Calabrese, E.; Cardoso, J.F.; 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.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R.D.; Davis, R.J.; de Bernardis, P.; de Zotti, G.; Delabrouille, J.; Delouis, J.M.; Desert, F.X.; 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.; Falgarone, E.; 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.; Guillet, V.; Hansen, F.K.; Hanson, D.; Harrison, D.L.; Helou, G.; Henrot-Versille, S.; Hernandez-Monteagudo, C.; Herranz, D.; Hivon, E.; Holmes, W.A.; Huffenberger, K.M.; Hurier, G.; Jaffe, A.H.; Jaffe, T.R.; Jewell, J.; Jones, W.C.; Juvela, M.; Keihanen, E.; Keskitalo, R.; Kisner, T.S.; Kneissl, R.; Knoche, J.; Knox, L.; Krachmalnicoff, N.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.M.; Lasenby, A.; Lattanzi, M.; Lawrence, C.R.; Leahy, J.P.; Leonardi, R.; Lesgourgues, J.; Levrier, F.; Liguori, M.; Lilje, P.B.; Linden-Vornle, M.; Lopez-Caniego, M.; Lubin, P.M.; Macias-Perez, J.F.; Maffei, B.; Maino, D.; Mandolesi, N.; Mangilli, A.; Maris, M.; Martin, P.G.; Martinez-Gonzalez, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschenes, M.A.; 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.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge, B.; 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.; Ponthieu, N.; Popa, L.; Pratt, G.W.; Prunet, S.; Puget, J.L.; Rachen, J.P.; Reach, W.T.; Rebolo, R.; Remazeilles, M.; Renault, C.; Renzi, A.; Ricciardi, S.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; d'Orfeuil, B.Rouille; Rubino-Martin, J.A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Savini, G.; Scott, D.; Soler, J.D.; 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.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vibert, L.; Vielva, P.; Villa, F.; Wade, L.A.; Wandelt, B.D.; Watson, R.; Wehus, I.K.; White, M.; White, S.D.M.; 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 intermediate results. 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The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes" property="og:title" /> <meta content="website" property="og:type" /> <meta content="https://cds.cern.ch/record/1757020" property="og:url" /> <meta name="twitter:image" content="https://cds.cern.ch/record/1757020/files/BB_Planck353_DX11d_detsets_mc_lin_MASK_FULL_2048_GAL_OFFICIAL_LARGE2.png" /> <meta property="og:image" content="https://cds.cern.ch/record/1757020/files/BB_Planck353_DX11d_detsets_mc_lin_MASK_FULL_2048_GAL_OFFICIAL_LARGE2.png" /> <meta property="og:image:secure_url" content="https://cds.cern.ch/record/1757020/files/BB_Planck353_DX11d_detsets_mc_lin_MASK_FULL_2048_GAL_OFFICIAL_LARGE2.png" /> <meta property="og:image" content="https://cds.cern.ch/record/1757020/files/BB_Planck353_DX11d_detsets_mc_masks_diff_lin_MASK_FULL_2048_GAL_OFFICIAL_LARGE2.png" /> <meta property="og:image:secure_url" 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/> <meta content="CERN Document Server" property="og:site_name" /> <meta content="The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100GHz. We exploit the Planck HFI polarization data from 100 to 353GHz to measure the dust angular power spectra $C_\ell^{EE,BB}$ over the range $40&lt;\ell&lt;600$ well away from the Galactic plane. These will bring new insights into interstellar dust physics and a precise determination of the level of contamination for CMB polarization experiments. We show that statistical properties of the emission can be characterized over large fractions of the sky using $C_\ell$. For the dust, they are well described by power laws in $\ell$ with exponents $\alpha^{EE,BB}=-2.42\pm0.02$. The amplitudes of the polarization $C_\ell$ vary with the average brightness in a way similar to the intensity ones. The dust polarization frequency dependence is consistent with modified blackbody emission with $\beta_d=1.59$ and $T_d=19.6$K. We find a systematic ratio between the amplitudes of the Galactic $B$- and $E$-modes of 0.5. We show that even in the faintest dust-emitting regions there are no &quot;clean&quot; windows where primordial CMB $B$-mode polarization could be measured without subtraction of dust emission. Finally, we investigate the level of dust polarization in the BICEP2 experiment field. Extrapolation of the Planck 353GHz data to 150GHz gives a dust power $\ell(\ell+1)C_\ell^{BB}/(2\pi)$ of $1.32\times10^{-2}\mu$K$_{CMB}^2$ over the $40&lt;\ell&lt;120$ range; the statistical uncertainty is $\pm0.29$ and there is an additional uncertainty (+0.28,-0.24) from the extrapolation, both in the same units. This is the same magnitude as reported by BICEP2 over this $\ell$ range, which highlights the need for assessment of the polarized dust signal even in the cleanest windows of the sky." property="og:description" /> <meta content="The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100GHz. We exploit the Planck HFI polarization data from 100 to 353GHz to measure the dust angular power spectra $C_\ell^{EE,BB}$ over the range $40&lt;\ell&lt;600$. These will bring new insights into interstellar dust physics and a precise determination of the level of contamination for CMB polarization experiments. We show that statistical properties of the emission can be characterized over large fractions of the sky using $C_\ell$. For the dust, they are well described by power laws in $\ell$ with exponents $\alpha^{EE,BB}=-2.42\pm0.02$. The amplitudes of the polarization $C_\ell$ vary with the average brightness in a way similar to the intensity ones. The dust polarization frequency dependence is consistent with modified blackbody emission with $\beta_d=1.59$ and $T_d=19.6$K. We find a systematic ratio between the amplitudes of the Galactic $B$- and $E$-modes of 0.5. We show that even in the faintest dust-emitting regions there are no &quot;clean&quot; windows where primordial CMB $B$-mode polarization could be measured without subtraction of dust emission. Finally, we investigate the level of dust polarization in the BICEP2 experiment field. Extrapolation of the Planck 353GHz data to 150GHz gives a dust power $\ell(\ell+1)C_\ell^{BB}/(2\pi)$ of $1.32\times10^{-2}\mu$K$_{CMB}^2$ over the $40&lt;\ell&lt;120$ range; the statistical uncertainty is $\pm0.29$ and there is an additional uncertainty (+0.28,-0.24) from the extrapolation, both in the same units. This is the same magnitude as reported by BICEP2 over this $\ell$ range, which highlights the need for assessment of the polarized dust signal. The present uncertainties will be reduced through an ongoing, joint analysis of the Planck and BICEP2 data sets." property="og:description" /> <meta content="arXiv" property="og:description" /> <meta content="The polarized thermal emission from diffuse Galactic dust is the main foreground presentin measurements of the polarization of the cosmic microwave background (CMB) atfrequencies above 100GHz. In this paper we exploit the uniqueness of thePlanck HFI polarization data from 100 to 353GHz to measure thepolarized dust angular power spectra C_l^EE and C_l^BB over themultipole range 40 well away from the Galactic plane. These measurements will bringnew insights into interstellar dust physics and allow a precise determination of the levelof contamination for CMB polarization experiments. Despite the non-Gaussian andanisotropic nature of Galactic dust, we show that general statistical properties of theemission can be characterized accurately over large fractions of the sky using angularpower spectra. The polarization power spectra of the dust are well described by power lawsin multipole, C_l ∝l^alpha, with exponentsalpha^EE,BB = -2.42 +- 0.02.The amplitudes of the polarization power spectra vary with the average brightness in a waysimilar to the intensity power spectra. The frequency dependence of the dust polarizationspectra is consistent with modified blackbody emission with beta_d = 1.59 andT_d = 19.6K down to the lowest Planck HFI frequencies. We find asystematic difference between the amplitudes of the Galactic B- and E-modes, C_l^BB/C_l^EE =0.5. We verify that these general properties are preserved towards highGalactic latitudes with low dust column densities. We show that even in the faintestdust-emitting regions there are no 'clean' windows in the sky where primordial CMBB-modepolarization measurements could be made without subtraction of foreground emission.Finally, we investigate the level of dust polarization in the specific field recentlytargeted by the BICEP2 experiment. Extrapolation of the Planck 353GHzdata to 150GHz gives a dust power 𝒟_l^BB =l(l+1)C_l^BB/(2pi) of 1.32 x 10^-2muK_CMB^2 over the multipole rangeof the primordial recombination bump (40); the statistical uncertainty is+- 0.29 x 10^-2muK_CMB^2 and there is anadditional uncertainty (+0.28, -0.24) x10^-2muK_CMB^2 from the extrapolation.This level is the same magnitude as reported by BICEP2 over this l range, which highlightsthe need for assessment of the polarized dust signal even in the cleanest windows of thesky." 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/1757020" 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 intermediate results. 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The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes </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/1757020/?ln=en">Information </a></li><li class=""><a href="/record/1757020/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="1757020"></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:1409.5738">arXiv:1409.5738</a></td></tr> <tr><td class="formatRecordLabel"> Title </td><td style="padding-left:5px;"><b>Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes</b></td></tr> <tr><td class="formatRecordLabel" style="vertical-align:top;">Related title</td><td style="padding-left:5px; ">Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes<br/></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 229 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=Adam%2C%20R.&ln=en">Adam, R.</a> (LPSC, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Ade%2C%20P.A.R.&ln=en">Ade, P.A.R.</a> (Cardiff U.) ; <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=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.) ; <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-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> (Toulouse III U. ; IRAP, Toulouse ; SISSA, Trieste) ; <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> (Toronto U.) ; <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. ; Paris U., VI-VII) ; <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=Bracco%2C%20A.&ln=en">Bracco, A.</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=Chamballu%2C%20A.&ln=en">Chamballu, A.</a> (DAPNIA, Saclay ; Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Chary%2C%20R.R.&ln=en">Chary, R.R.</a> (Caltech) ; <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=Colombi%2C%20S.&ln=en">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=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=Couchot%2C%20F.&ln=en">Couchot, F.</a> (Orsay) ; <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=Curto%2C%20A.&ln=en">Curto, A.</a> (Cambridge U. ; Cantabria Inst. of Phys.) ; <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%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=Delouis%2C%20J.M.&ln=en">Delouis, J.M.</a> (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <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=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> (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=Falgarone%2C%20E.&ln=en">Falgarone, E.</a> (LERMA, Ivry) ; <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> (Paris, Inst. Astrophys.) ; <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=Ghosh%2C%20T.&ln=en">Ghosh, T.</a> (Orsay) ; <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=Giraud-Heraud%2C%20Y.&ln=en">Giraud-Heraud, Y.</a> (APC, Paris) ; <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> (Cantabria Inst. of Phys. ; SISSA, Trieste) ; <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=Guillet%2C%20V.&ln=en">Guillet, V.</a> (Orsay) ; <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=Hanson%2C%20D.&ln=en">Hanson, D.</a> (Rutherford ; Caltech ; Toronto 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=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=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=Jaffe%2C%20T.R.&ln=en">Jaffe, T.R.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Jewell%2C%20J.&ln=en">Jewell, J.</a> (Caltech) ; <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=Kisner%2C%20T.S.&ln=en">Kisner, T.S.</a> (LBL, Berkeley) ; <a href="https://cds.cern.ch/search?f=author&p=Kneissl%2C%20R.&ln=en">Kneissl, R.</a> (European Southern Obs., Chile) ; <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=Krachmalnicoff%2C%20N.&ln=en">Krachmalnicoff, N.</a> (Milan U.) ; <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> (Orsay) ; <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=Leahy%2C%20J.P.&ln=en">Leahy, J.P.</a> (Manchester U.) ; <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> (CERN ; LPHE, Lausanne ; Savoie U.) ; <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=Liguori%2C%20M.&ln=en">Liguori, M.</a> (Padua U.) ; <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=Linden-Vornle%2C%20M.&ln=en">Linden-Vornle, M.</a> (Denmark, Tech. U.) ; <a href="https://cds.cern.ch/search?f=author&p=Lopez-Caniego%2C%20M.&ln=en">Lopez-Caniego, M.</a> (Cantabria Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Lubin%2C%20P.M.&ln=en">Lubin, P.M.</a> (UC, Santa Barbara) ; <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=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. ; ASI, Rome ; Ferrara U.) ; <a href="https://cds.cern.ch/search?f=author&p=Mangilli%2C%20A.&ln=en">Mangilli, A.</a> (Paris, Inst. Astrophys.) ; <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> (Toronto U.) ; <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.) ; <a href="https://cds.cern.ch/search?f=author&p=Mazzotta%2C%20P.&ln=en">Mazzotta, P.</a> (Rome U.) ; <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=Mendes%2C%20L.&ln=en">Mendes, L.</a> (ESA, Madrid) ; <a href="https://cds.cern.ch/search?f=author&p=Mennella%2C%20A.&ln=en">Mennella, A.</a> (Milan U. ; Brera Observ.) ; <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=Mitra%2C%20S.&ln=en">Mitra, S.</a> (Pune U. ; Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Miville-Deschenes%2C%20M.A.&ln=en">Miville-Deschenes, M.A.</a> (Orsay ; Toronto U.) ; <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=Moss%2C%20A.&ln=en">Moss, A.</a> (Nottingham U.) ; <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=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> (Rome 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=Netterfield%2C%20C.B.&ln=en">Netterfield, C.B.</a> (Toronto U.) ; <a href="https://cds.cern.ch/search?f=author&p=Norgaard-Nielsen%2C%20H.U.&ln=en">Norgaard-Nielsen, H.U.</a> (Denmark, Tech. 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Space Science) ; <a href="https://cds.cern.ch/search?f=author&p=Pratt%2C%20G.W.&ln=en">Pratt, G.W.</a> (DAPNIA, Saclay) ; <a href="https://cds.cern.ch/search?f=author&p=Prunet%2C%20S.&ln=en">Prunet, S.</a> (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; <a href="https://cds.cern.ch/search?f=author&p=Puget%2C%20J.L.&ln=en">Puget, J.L.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Rachen%2C%20J.P.&ln=en">Rachen, J.P.</a> (Nijmegen U. ; Garching, Max Planck Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Reach%2C%20W.T.&ln=en">Reach, W.T.</a> (Universities Space Research Assoc.) ; <a href="https://cds.cern.ch/search?f=author&p=Rebolo%2C%20R.&ln=en">Rebolo, R.</a> (IAC, La Laguna ; CSIC, Madrid ; Laguna U., Tenerife) ; <a href="https://cds.cern.ch/search?f=author&p=Remazeilles%2C%20M.&ln=en">Remazeilles, M.</a> (Manchester U. ; Orsay ; APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Renault%2C%20C.&ln=en">Renault, C.</a> (LPSC, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Renzi%2C%20A.&ln=en">Renzi, A.</a> (Rome U. ; INFN, Rome) ; <a href="https://cds.cern.ch/search?f=author&p=Ricciardi%2C%20S.&ln=en">Ricciardi, S.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Ristorcelli%2C%20I.&ln=en">Ristorcelli, I.</a> (Toulouse III U. ; IRAP, Toulouse) ; <a href="https://cds.cern.ch/search?f=author&p=Rocha%2C%20G.&ln=en">Rocha, G.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Rosset%2C%20C.&ln=en">Rosset, C.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Rossetti%2C%20M.&ln=en">Rossetti, M.</a> (Milan U. ; Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Roudier%2C%20G.&ln=en">Roudier, G.</a> (APC, Paris ; LERMA, Ivry ; Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=d%27Orfeuil%2C%20B.Rouille&ln=en">d'Orfeuil, B.Rouille</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Rubino-Martin%2C%20J.A.&ln=en">Rubino-Martin, J.A.</a> (IAC, La Laguna ; Laguna U., Tenerife) ; <a href="https://cds.cern.ch/search?f=author&p=Rusholme%2C%20B.&ln=en">Rusholme, B.</a> (Caltech) ; <a href="https://cds.cern.ch/search?f=author&p=Sandri%2C%20M.&ln=en">Sandri, M.</a> (Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Santos%2C%20D.&ln=en">Santos, D.</a> (LPSC, Grenoble) ; <a href="https://cds.cern.ch/search?f=author&p=Savelainen%2C%20M.&ln=en">Savelainen, M.</a> (Helsinki U. ; Helsinki Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Savini%2C%20G.&ln=en">Savini, G.</a> (University Coll. London) ; <a href="https://cds.cern.ch/search?f=author&p=Scott%2C%20D.&ln=en">Scott, D.</a> (British Columbia U.) ; <a href="https://cds.cern.ch/search?f=author&p=Soler%2C%20J.D.&ln=en">Soler, J.D.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Spencer%2C%20L.D.&ln=en">Spencer, L.D.</a> (Cardiff U.) ; <a href="https://cds.cern.ch/search?f=author&p=Stolyarov%2C%20V.&ln=en">Stolyarov, V.</a> (Cambridge U. ; Cambridge U., KICC ; Stavropol, Astrophys. Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Stompor%2C%20R.&ln=en">Stompor, R.</a> (APC, Paris) ; <a href="https://cds.cern.ch/search?f=author&p=Sudiwala%2C%20R.&ln=en">Sudiwala, R.</a> (Cardiff U.) ; <a href="https://cds.cern.ch/search?f=author&p=Sunyaev%2C%20R.&ln=en">Sunyaev, R.</a> (Garching, Max Planck Inst. ; Moscow, Space Res. Inst.) ; <a href="https://cds.cern.ch/search?f=author&p=Sutton%2C%20D.&ln=en">Sutton, D.</a> (Cambridge U., Inst. of Astron. ; Cambridge U., KICC) ; <a href="https://cds.cern.ch/search?f=author&p=Suur-Uski%2C%20A.S.&ln=en">Suur-Uski, A.S.</a> (Helsinki U. ; Helsinki Inst. of Phys.) ; <a href="https://cds.cern.ch/search?f=author&p=Sygnet%2C%20J.F.&ln=en">Sygnet, J.F.</a> (Paris, Inst. Astrophys.) ; <a href="https://cds.cern.ch/search?f=author&p=Tauber%2C%20J.A.&ln=en">Tauber, J.A.</a> (ESTEC, Noordwijk) ; <a href="https://cds.cern.ch/search?f=author&p=Terenzi%2C%20L.&ln=en">Terenzi, L.</a> (Facolta di Ingegneria, Rome ; Bologna Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Tomasi%2C%20M.&ln=en">Tomasi, M.</a> (Milan U. ; Brera Observ.) ; <a href="https://cds.cern.ch/search?f=author&p=Tristram%2C%20M.&ln=en">Tristram, M.</a> (Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Tucci%2C%20M.&ln=en">Tucci, M.</a> (Geneva U. ; Orsay) ; <a href="https://cds.cern.ch/search?f=author&p=Tuovinen%2C%20J.&ln=en">Tuovinen, J.</a> (Trinity Coll., Dublin) ; <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=Vibert%2C%20L.&ln=en">Vibert, L.</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=Watson%2C%20R.&ln=en">Watson, R.</a> (Manchester U.) ; <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=White%2C%20M.&ln=en">White, M.</a> (UC, Berkeley) ; <a href="https://cds.cern.ch/search?f=author&p=White%2C%20S.D.M.&ln=en">White, S.D.M.</a> (Garching, Max Planck Inst.) ; <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;">2016-02-09</td></tr> <tr><td class="formatRecordLabel"> Imprint </td><td style="padding-left:5px;">19 Sep 2014</td></tr> <tr><td class="formatRecordLabel"> Number of pages </td><td style="padding-left:5px;">25</td></tr> <tr><td class="formatRecordLabel"> Note </td><td style="padding-left:5px;">25 pages, 25 figures, accepted in A&A</td></tr> <tr><td class="formatRecordLabel"> In: </td><td style="padding-left:5px;"><a href="http://dx.doi.org/10.1051/0004-6361/201425034"><i>Astron. Astrophys.</i> 586 (2016) A133</a> </a></td></tr> <tr><td class="formatRecordLabel"> DOI </td><td style="padding-left:5px;"><a href="http://dx.doi.org/10.1051/0004-6361/201425034" title="DOI" target="_blank">10.1051/0004-6361/201425034</a> <tr><td class="formatRecordLabel"> Subject category </td><td style="padding-left:5px;">Astrophysics and Astronomy</td></tr> <tr><td class="formatRecordLabel"> Accelerator/Facility, Experiment </td><td style="padding-left:5px;"><a href="https://cds.cern.ch/search?p=PLANCK%20RE24&f=693__e">PLANCK RE24</a></td></tr> <tr><td class="formatRecordLabel"> Abstract </td><td style="padding-left:5px;">The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100GHz. We exploit the Planck HFI polarization data from 100 to 353GHz to measure the dust angular power spectra $C_\ell^{EE,BB}$ over the range $40<\ell<600$. These will bring new insights into interstellar dust physics and a precise determination of the level of contamination for CMB polarization experiments. We show that statistical properties of the emission can be characterized over large fractions of the sky using $C_\ell$. For the dust, they are well described by power laws in $\ell$ with exponents $\alpha^{EE,BB}=-2.42\pm0.02$. The amplitudes of the polarization $C_\ell$ vary with the average brightness in a way similar to the intensity ones. The dust polarization frequency dependence is consistent with modified blackbody emission with $\beta_d=1.59$ and $T_d=19.6$K. We find a systematic ratio between the amplitudes of the Galactic $B$- and $E$-modes of 0.5. We show that even in the faintest dust-emitting regions there are no "clean" windows where primordial CMB $B$-mode polarization could be measured without subtraction of dust emission. Finally, we investigate the level of dust polarization in the BICEP2 experiment field. Extrapolation of the Planck 353GHz data to 150GHz gives a dust power $\ell(\ell+1)C_\ell^{BB}/(2\pi)$ of $1.32\times10^{-2}\mu$K$_{CMB}^2$ over the $40<\ell<120$ range; the statistical uncertainty is $\pm0.29$ and there is an additional uncertainty (+0.28,-0.24) from the extrapolation, both in the same units. This is the same magnitude as reported by BICEP2 over this $\ell$ range, which highlights the need for assessment of the polarized dust signal. The present uncertainties will be reduced through an ongoing, joint analysis of the Planck and BICEP2 data sets.</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/1757020/plots#0"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/1757020/files/maskall.png" title=" Masks and complementary selected large {\window}s that retain fractional coverage of the sky \fsky from 0.8 to 0.3 (see details in Sect.~\ref{intlat_masks}). The darkest blue is the CO mask, whose complement is a selected \window\ with $\fsky = 0.8$. In increments of $f_{\rm sky}=0.1$, the retained {\window}s can be identified by the colours dark red (0.3) to dark blue (0.8), inclusively. Also shown is the (unapodized) point source mask used." width="200px"/></a> <a href="/record/1757020/plots#1"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/1757020/files/Syste_Dlspectra_DX11_EE_Imasks_NewPS.png" title=" \footnotesize \Planck\ HFI 353\,GHz \dlee\ (red, top) and \dlbb\ (blue, bottom) power spectra (in $\mu$K$_{\rm CMB}^2$) computed on three of the selected \lwdpref\ analysis regions that have $\fsky=0.3$ (circles, lightest), $\fsky=0.5$ (diamonds, medium) and $\fsky=0.7$ (squares, darkest). The best-fit power laws in $\ell$ are displayed for each spectrum as a dashed line of the corresponding colour. The \Planck\ 2013 best-fit $\Lambda$CDM \dlee\ expectation \citep{planck2013-p11} and the corresponding $r=0.2$ \dlbb\ CMB model are displayed as solid black lines; the rise for $\ell >200$ is from the lensing contribution. In the lower parts of each panel, the global estimates of the power spectra of the systematic effects responsible for intensity-to-polarization leakage (Sect.~\ref{systematics}) are displayed in different shades of grey, with the same symbols to identify the three {\window}s. Finally, absolute values of the null-test spectra anticipated in Sect.~\ref{systematics}, computed here from the cross-spectra of the HalfRing/DetSet differences (see text), are represented as dashed-dotted, dashed, and dotted grey lines for the three \lwdpref\ {\window}s." width="200px"/></a> <a href="/record/1757020/plots#2"><img style="vertical-align:middle;" src="https://cds.cern.ch/record/1757020/files/Syste_Dlspectra_DX11_BB_Imasks_NewPS.png" title=" \footnotesize \Planck\ HFI 353\,GHz \dlee\ (red, top) and \dlbb\ (blue, bottom) power spectra (in $\mu$K$_{\rm CMB}^2$) computed on three of the selected \lwdpref\ analysis regions that have $\fsky=0.3$ (circles, lightest), $\fsky=0.5$ (diamonds, medium) and $\fsky=0.7$ (squares, darkest). The best-fit power laws in $\ell$ are displayed for each spectrum as a dashed line of the corresponding colour. The \Planck\ 2013 best-fit $\Lambda$CDM \dlee\ expectation \citep{planck2013-p11} and the corresponding $r=0.2$ \dlbb\ CMB model are displayed as solid black lines; the rise for $\ell >200$ is from the lensing contribution. In the lower parts of each panel, the global estimates of the power spectra of the systematic effects responsible for intensity-to-polarization leakage (Sect.~\ref{systematics}) are displayed in different shades of grey, with the same symbols to identify the three {\window}s. Finally, absolute values of the null-test spectra anticipated in Sect.~\ref{systematics}, computed here from the cross-spectra of the HalfRing/DetSet differences (see text), are represented as dashed-dotted, dashed, and dotted grey lines for the three \lwdpref\ {\window}s." width="200px"/></a> <a href='/record/1757020/plots'>Show more plots</a></div></div><br /> <br/>Corresponding record in: <a href="http://inspirehep.net/record/1318318">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 2014-09-22, last modified 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=en&p=recid%3A1757020&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/1757020/files/arXiv:1409.5738.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://www.nature.com/news/full-galaxy-dust-map-muddles-search-for-gravitational-waves-1.15975"><img style="border:none" src="/img/file-icon-text-12x16.gif" alt="Download fulltext"/>Nature article</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=1757020">Add to personal basket</a></li> <li>Export as <a style="text-decoration:underline;font-weight:normal" href="/record/1757020/export/hx?ln=en">BibTeX</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1757020/export/hm?ln=en">MARC</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1757020/export/xm?ln=en">MARCXML</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1757020/export/xd?ln=en">DC</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1757020/export/xe?ln=en">EndNote</a>,  <a style="text-decoration:underline;font-weight:normal" href="/record/1757020/export/xn?ln=en">NLM</a>, <a style="text-decoration:underline;font-weight:normal" href="/record/1757020/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/1409.5738/add'); $('#bookmark_sciencewise').bookmark({sites: ['sciencewise']}); $('#bookmark').bookmark({ sites: ['facebook', 'twitter', 'linkedin', 'google_plusone'], icons: '/img/bookmarks.png', url: 'https://cds.cern.ch/record/1757020', addEmail: true, title: "Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes", description: "The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100GHz. We exploit the Planck HFI polarization data from 100 to 353GHz to measure the dust angular power spectra $C_\\ell^{EE,BB}$ over the range $40<\\ell<600$. These will bring new insights into interstellar dust physics and a precise determination of the level of contamination for CMB polarization experiments. We show that statistical properties of the emission can be characterized over large fractions of the sky using $C_\\ell$. For the dust, they are well described by power laws in $\\ell$ with exponents $\\alpha^{EE,BB}=-2.42\\pm0.02$. The amplitudes of the polarization $C_\\ell$ vary with the average brightness in a way similar to the intensity ones. The dust polarization frequency dependence is consistent with modified blackbody emission with $\\beta_d=1.59$ and $T_d=19.6$K. We find a systematic ratio between the amplitudes of the Galactic $B$- and $E$-modes of 0.5. We show that even in the faintest dust-emitting regions there are no \"clean\" windows where primordial CMB $B$-mode polarization could be measured without subtraction of dust emission. Finally, we investigate the level of dust polarization in the BICEP2 experiment field. Extrapolation of the Planck 353GHz data to 150GHz gives a dust power $\\ell(\\ell+1)C_\\ell^{BB}/(2\\pi)$ of $1.32\\times10^{-2}\\mu$K$_{CMB}^2$ over the $40<\\ell<120$ range; the statistical uncertainty is $\\pm0.29$ and there is an additional uncertainty (+0.28,-0.24) from the extrapolation, both in the same units. This is the same magnitude as reported by BICEP2 over this $\\ell$ range, which highlights the need for assessment of the polarized dust signal. The present uncertainties will be reduced through an ongoing, joint analysis of the Planck and BICEP2 data sets." }); // ]]> </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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