Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes - CERN Document Server

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Report number	arXiv:1409.5738
Title	Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes
Related title	Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes
Author(s)	Adam, R. (LPSC, Grenoble) ; Ade, P.A.R. (Cardiff U.) ; Aghanim, N. (Orsay) ; Arnaud, M. (DAPNIA, Saclay) ; Aumont, J. (Orsay) ; Baccigalupi, C. (SISSA, Trieste) ; Banday, A.J. (Toulouse III U. ; IRAP, Toulouse) ; Barreiro, R.B. (Cantabria Inst. of Phys.) ; Bartlett, J.G. (APC, Paris ; Caltech) ; Bartolo, N. (Padua U.) ; Battaner, E. (Granada U.) ; Benabed, K. (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; Benoit-Levy, A. (University Coll. London ; Paris, Inst. Astrophys. ; Paris U., VI-VII) ; Bernard, J.P. (Toulouse III U. ; IRAP, Toulouse) ; Bersanelli, M. (Milan U. ; Brera Observ.) ; Bielewicz, P. (Toulouse III U. ; IRAP, Toulouse ; SISSA, Trieste) ; Bonaldi, A. (Manchester U.) ; Bonavera, L. (Cantabria Inst. of Phys.) ; Bond, J.R. (Toronto U.) ; Borrill, J. (LBL, Berkeley ; UC, Berkeley) ; Bouchet, F.R. (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; Boulanger, F. (Orsay) ; Bracco, A. (Orsay) ; Bucher, M. (APC, Paris) ; Burigana, C. (Bologna Observ. ; Ferrara U. ; INFN, Bologna) ; Butler, R.C. (Bologna Observ.) ; Calabrese, E. (Oxford U.) ; Cardoso, J.F. (LTCI, Paris ; APC, Paris ; Paris, Inst. Astrophys.) ; Catalano, A. (LPSC, Grenoble ; LERMA, Ivry) ; Challinor, A. (Cambridge U., Inst. of Astron. ; Cambridge U., KICC ; Cambridge U., DAMTP) ; Chamballu, A. (DAPNIA, Saclay ; Orsay) ; Chary, R.R. (Caltech) ; Chiang, H.C. (Princeton U. ; KwaZulu Natal U.) ; Christensen, P.R. (Bohr Inst.) ; Clements, D.L. (Imperial Coll., London) ; Colombi, S. (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; Colombo, L.P.L. (UCLA ; Caltech) ; Combet, C. (LPSC, Grenoble) ; Couchot, F. (Orsay) ; Coulais, A. (LERMA, Ivry) ; Curto, A. (Cambridge U. ; Cantabria Inst. of Phys.) ; Cuttaia, F. (Bologna Observ.) ; Danese, L. (SISSA, Trieste) ; Davies, R.D. (Manchester U.) ; Davis, R.J. (Manchester U.) ; de Bernardis, P. (Rome U.) ; de Zotti, G. (Padua Observ. ; SISSA, Trieste) ; Delabrouille, J. (APC, Paris) ; Delouis, J.M. (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; Desert, F.X. (Grenoble Observ.) ; Dickinson, C. (Manchester U.) ; Diego, J.M. (Cantabria Inst. of Phys.) ; Dolag, K. (Munich U. ; Garching, Max Planck Inst.) ; Dole, H. (Orsay ; IUF, Paris) ; Donzelli, S. (Brera Observ.) ; Dore, O. (Caltech) ; Douspis, M. (Orsay) ; Ducout, A. (Paris, Inst. Astrophys. ; Imperial Coll., London) ; Dunkley, J. (Oxford U.) ; Dupac, X. (ESA, Madrid) ; Efstathiou, G. (Cambridge U., Inst. of Astron.) ; Elsner, F. (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; Ensslin, T.A. (Garching, Max Planck Inst.) ; Eriksen, H.K. (Oslo U.) ; Falgarone, E. (LERMA, Ivry) ; Finelli, F. (Bologna Observ. ; INFN, Bologna) ; Forni, O. (Toulouse III U. ; IRAP, Toulouse) ; Frailis, M. (Trieste Observ.) ; Fraisse, A.A. (Princeton U.) ; Franceschi, E. (Bologna Observ.) ; Frejsel, A. (Bohr Inst.) ; Galeotta, S. (Trieste Observ.) ; Galli, S. (Paris, Inst. Astrophys.) ; Ganga, K. (APC, Paris) ; Ghosh, T. (Orsay) ; Giard, M. (Toulouse III U. ; IRAP, Toulouse) ; Giraud-Heraud, Y. (APC, Paris) ; Gjerlow, E. (Oslo U.) ; Gonzalez-Nuevo, J. (Cantabria Inst. of Phys. ; SISSA, Trieste) ; Gorski, K.M. (Caltech ; Warsaw U.) ; Gratton, S. (Cambridge U., KICC ; Cambridge U., Inst. of Astron.) ; Gregorio, A. (Trieste U. ; Trieste Observ. ; INFN, Trieste) ; Gruppuso, A. (Bologna Observ.) ; Guillet, V. (Orsay) ; Hansen, F.K. (Oslo U.) ; Hanson, D. (Rutherford ; Caltech ; Toronto U.) ; Harrison, D.L. (Cambridge U., Inst. of Astron. ; Cambridge U., KICC) ; Helou, G. (Caltech) ; Henrot-Versille, S. (Orsay) ; Hernandez-Monteagudo, C. (CEFCA, Teruel ; Garching, Max Planck Inst.) ; Herranz, D. (Cantabria Inst. of Phys.) ; Hivon, E. (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; Holmes, W.A. (Caltech) ; Huffenberger, K.M. (Florida State U.) ; Hurier, G. (Orsay) ; Jaffe, A.H. (Imperial Coll., London) ; Jaffe, T.R. (Toulouse III U. ; IRAP, Toulouse) ; Jewell, J. (Caltech) ; Jones, W.C. (Princeton U.) ; Juvela, M. (Helsinki U.) ; Keihanen, E. (Helsinki U.) ; Keskitalo, R. (LBL, Berkeley) ; Kisner, T.S. (LBL, Berkeley) ; Kneissl, R. (European Southern Obs., Chile) ; Knoche, J. (Garching, Max Planck Inst.) ; Knox, L. (UC, Davis) ; Krachmalnicoff, N. (Milan U.) ; Kunz, M. (Geneva U. ; Orsay ; African Inst. Math. Sci., Cape Town) ; Kurki-Suonio, H. (Helsinki U. ; Helsinki Inst. of Phys.) ; Lagache, G. (Orsay) ; Lamarre, J.M. (LERMA, Ivry) ; Lasenby, A. (Cambridge U. ; Cambridge U., KICC) ; Lattanzi, M. (Ferrara U.) ; Lawrence, C.R. (Caltech) ; Leahy, J.P. (Manchester U.) ; Leonardi, R. (ESA, Madrid) ; Lesgourgues, J. (CERN ; LPHE, Lausanne ; Savoie U.) ; Levrier, F. (LERMA, Ivry) ; Liguori, M. (Padua U.) ; Lilje, P.B. (Oslo U.) ; Linden-Vornle, M. (Denmark, Tech. U.) ; Lopez-Caniego, M. (Cantabria Inst. of Phys.) ; Lubin, P.M. (UC, Santa Barbara) ; Macias-Perez, J.F. (LPSC, Grenoble) ; Maffei, B. (Manchester U.) ; Maino, D. (Milan U. ; Brera Observ.) ; Mandolesi, N. (Bologna Observ. ; ASI, Rome ; Ferrara U.) ; Mangilli, A. (Paris, Inst. Astrophys.) ; Maris, M. (Trieste Observ.) ; Martin, P.G. (Toronto U.) ; Martinez-Gonzalez, E. (Cantabria Inst. of Phys.) ; Masi, S. (Rome U.) ; Matarrese, S. (Padua U.) ; Mazzotta, P. (Rome U.) ; Melchiorri, A. (Rome U. ; INFN, Rome) ; Mendes, L. (ESA, Madrid) ; Mennella, A. (Milan U. ; Brera Observ.) ; Migliaccio, M. (Cambridge U., Inst. of Astron. ; Cambridge U., KICC) ; Mitra, S. (Pune U. ; Caltech) ; Miville-Deschenes, M.A. (Orsay ; Toronto U.) ; Moneti, A. (Paris, Inst. Astrophys.) ; Montier, L. (Toulouse III U. ; IRAP, Toulouse) ; Morgante, G. (Bologna Observ.) ; Mortlock, D. (Imperial Coll., London) ; Moss, A. (Nottingham U.) ; Munshi, D. (Cardiff U.) ; Murphy, J.A. (NUIM, Maynooth) ; Naselsky, P. (Bohr Inst.) ; Nati, F. (Rome U.) ; Natoli, P. (Ferrara U. ; INFN, Rome2 ; Bologna Observ.) ; Netterfield, C.B. (Toronto U.) ; Norgaard-Nielsen, H.U. (Denmark, Tech. U.) ; Noviello, F. (Manchester U.) ; Novikov, D. (Imperial Coll., London) ; Novikov, I. (Bohr Inst.) ; Pagano, L. (Rome U. ; INFN, Rome) ; Pajot, F. (Orsay) ; Paladini, R. (Caltech) ; Paoletti, D. (Bologna Observ. ; INFN, Bologna) ; Partridge, B. (Haverford Coll.) ; Pasian, F. (Trieste Observ.) ; Patanchon, G. (APC, Paris) ; Pearson, T.J. (Caltech) ; Perdereau, O. (Orsay) ; Perotto, L. (LPSC, Grenoble) ; Perrotta, F. (SISSA, Trieste) ; Pettorino, V. (Heidelberg U.) ; Piacentini, F. (Rome U.) ; Piat, M. (APC, Paris) ; Pierpaoli, E. (UCLA) ; Pietrobon, D. (Caltech) ; Plaszczynski, S. (Orsay) ; Pointecouteau, E. (Toulouse III U. ; IRAP, Toulouse) ; Polenta, G. (INFN, Rome2 ; Rome Observ.) ; Ponthieu, N. (Orsay ; Grenoble Observ.) ; Popa, L. (Bucharest, Inst. Space Science) ; Pratt, G.W. (DAPNIA, Saclay) ; Prunet, S. (Paris, Inst. Astrophys. ; Paris U., VI-VII) ; Puget, J.L. (Orsay) ; Rachen, J.P. (Nijmegen U. ; Garching, Max Planck Inst.) ; Reach, W.T. (Universities Space Research Assoc.) ; Rebolo, R. (IAC, La Laguna ; CSIC, Madrid ; Laguna U., Tenerife) ; Remazeilles, M. (Manchester U. ; Orsay ; APC, Paris) ; Renault, C. (LPSC, Grenoble) ; Renzi, A. (Rome U. ; INFN, Rome) ; Ricciardi, S. (Bologna Observ.) ; Ristorcelli, I. (Toulouse III U. ; IRAP, Toulouse) ; Rocha, G. (Caltech) ; Rosset, C. (APC, Paris) ; Rossetti, M. (Milan U. ; Brera Observ.) ; Roudier, G. (APC, Paris ; LERMA, Ivry ; Caltech) ; d'Orfeuil, B.Rouille (Orsay) ; Rubino-Martin, J.A. (IAC, La Laguna ; Laguna U., Tenerife) ; Rusholme, B. (Caltech) ; Sandri, M. (Bologna Observ.) ; Santos, D. (LPSC, Grenoble) ; Savelainen, M. (Helsinki U. ; Helsinki Inst. of Phys.) ; Savini, G. (University Coll. London) ; Scott, D. (British Columbia U.) ; Soler, J.D. (Orsay) ; Spencer, L.D. (Cardiff U.) ; Stolyarov, V. (Cambridge U. ; Cambridge U., KICC ; Stavropol, Astrophys. Observ.) ; Stompor, R. (APC, Paris) ; Sudiwala, R. (Cardiff U.) ; Sunyaev, R. (Garching, Max Planck Inst. ; Moscow, Space Res. Inst.) ; Sutton, D. (Cambridge U., Inst. of Astron. ; Cambridge U., KICC) ; Suur-Uski, A.S. (Helsinki U. ; Helsinki Inst. of Phys.) ; Sygnet, J.F. (Paris, Inst. Astrophys.) ; Tauber, J.A. (ESTEC, Noordwijk) ; Terenzi, L. (Facolta di Ingegneria, Rome ; Bologna Observ.) ; Tomasi, M. (Milan U. ; Brera Observ.) ; Tristram, M. (Orsay) ; Tucci, M. (Geneva U. ; Orsay) ; Tuovinen, J. (Trinity Coll., Dublin) ; Valenziano, L. (Bologna Observ.) ; Valiviita, J. (Helsinki U. ; Helsinki Inst. of Phys.) ; Van Tent, B. (Orsay) ; Vibert, L. (Orsay) ; Vielva, P. (Cantabria Inst. of Phys.) ; Villa, F. (Bologna Observ.) ; Wade, L.A. (Caltech) ; Wandelt, B.D. (Paris, Inst. Astrophys. ; Paris U., VI-VII ; Illinois U., Urbana) ; Watson, R. (Manchester U.) ; Wehus, I.K. (Caltech) ; White, M. (UC, Berkeley) ; White, S.D.M. (Garching, Max Planck Inst.) ; Yvon, D. (DAPNIA, Saclay) ; Zacchei, A. (Trieste Observ.) ; Zonca, A. (UC, Santa Barbara)
Publication	2016-02-09
Imprint	19 Sep 2014
Number of pages	25
Note	25 pages, 25 figures, accepted in A&A
In:	Astron. Astrophys. 586 (2016) A133
DOI	10.1051/0004-6361/201425034
Subject category	Astrophysics and Astronomy
Accelerator/Facility, Experiment	PLANCK RE24
Abstract	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.
Copyright/License	arXiv nonexclusive-distrib. 1.0

$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.$ $\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"/> $\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"/> Show more plots

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