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

Planck Collaboration; R Adam; P A R Ade; N Aghanim; M Arnaud; J Aumont; C Baccigalupi; A J Banday; R B Barreiro; J G Bartlett; N Bartolo; E Battaner; K Benabed; A Benoit-L??vy; J-P Bernard; M Bersanelli; P Bielewicz; A Bonaldi; L Bonavera; J R Bond; J Borrill; F R Bouchet; F Boulanger; A Bracco; M Bucher; C Burigana; R C Butler; E Calabrese; J-F Cardoso; A Catalano; A Challinor; A Chamballu; R-R Chary; H C Chiang; P R Christensen; D L Clements; S Colombi; L P L Colombo; C Combet; F Couchot; A Coulais; B P Crill; A Curto; F Cuttaia; L Danese; R D Davies; R J Davis; P de Bernardis; G de Zotti; J Delabrouille; J-M Delouis; F-X D??sert; C Dickinson; J M Diego; K Dolag; H Dole; S Donzelli; O Dor??; M Douspis; A Ducout; J Dunkley; X Dupac; G Efstathiou; F Elsner; T A En??lin; H K Eriksen; E Falgarone; F Finelli; O Forni; M Frailis; A A Fraisse; E Franceschi; A Frejsel; S Galeotta; S Galli; K Ganga; T Ghosh; M Giard; Y Giraud-H??raud; E Gjerl??w; J Gonz??lez-Nuevo; K M G??rski; S Gratton; A Gregorio; A Gruppuso; V Guillet; F K Hansen; D Hanson; D L Harrison; G Helou; S Henrot-Versill??; C Hern??ndez-Monteagudo; D Herranz; E Hivon; M Hobson; W A Holmes; K M Huffenberger; G Hurier; A H Jaffe; T R Jaffe; J Jewell; W C Jones; M Juvela; E Keih??nen; R Keskitalo; T S Kisner; R Kneissl; J Knoche; L Knox; N Krachmalnicoff; M Kunz; H Kurki-Suonio; G Lagache; J-M Lamarre; A Lasenby; M Lattanzi; C R Lawrence; J P Leahy; R Leonardi; J Lesgourgues; F Levrier; M Liguori; P B Lilje; M Linden-V??rnle; M L??pez-Caniego; P M Lubin; J F Mac??as-P??rez; B Maffei; D Maino; N Mandolesi; A Mangilli; M Maris; P G Martin; E Mart??nez-Gonz??lez; S Masi; S Matarrese; P Mazzotta; A Melchiorri; L Mendes; A Mennella; M Migliaccio; S Mitra; M-A Miville-Desch??nes; A Moneti; L Montier; G Morgante; D Mortlock; A Moss; D Munshi; J A Murphy; P Naselsky; F Nati; P Natoli; C B Netterfield; H U N??rgaard-Nielsen; F Noviello; D Novikov; I Novikov; L Pagano; F Pajot; R Paladini; D Paoletti; B Partridge; F Pasian; G Patanchon; T J Pearson; O Perdereau; L Perotto; F Perrotta; V Pettorino; F Piacentini; M Piat; E Pierpaoli; D Pietrobon; S Plaszczynski; E Pointecouteau; G Polenta; N Ponthieu; L Popa; G W Pratt; S Prunet; J-L Puget; J P Rachen; W T Reach; R Rebolo; M Remazeilles; C Renault; A Renzi; S Ricciardi; I Ristorcelli; G Rocha; C Rosset; M Rossetti; G Roudier; B Rouill?? d'Orfeuil; J A Rubi??o-Mart??n; B Rusholme; M Sandri; D Santos; M Savelainen; G Savini; D Scott; J D Soler; L D Spencer; V Stolyarov; R Stompor; R Sudiwala; R Sunyaev; D Sutton; A-S Suur-Uski; J-F Sygnet; J A Tauber; L Terenzi; L Toffolatti; M Tomasi; M Tristram; M Tucci; J Tuovinen; L Valenziano; J Valiviita; B Van Tent; L Vibert; P Vielva; F Villa; L A Wade; B D Wandelt; R Watson; I K Wehus; M White; S D M White; D Yvon; A Zacchei; A Zonca

doi:10.1051/0004-6361/201425034

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

Planck Collaboration, R Adam, P A R Ade, N Aghanim, M Arnaud, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, J G Bartlett, N Bartolo, E Battaner, K Benabed, A Benoit-L??vy, J-P Bernard, M Bersanelli, P Bielewicz, A Bonaldi, L Bonavera, J R BondJ Borrill, F R Bouchet, F Boulanger, A Bracco, M Bucher, C Burigana, R C Butler, E Calabrese, J-F Cardoso, A Catalano, A Challinor, A Chamballu, R-R Chary, H C Chiang, P R Christensen, D L Clements, S Colombi, L P L Colombo, C Combet, F Couchot, A Coulais, B P Crill, A Curto, F Cuttaia, L Danese, R D Davies, R J Davis, P de Bernardis, G de Zotti, J Delabrouille, J-M Delouis, F-X D??sert, C Dickinson, J M Diego, K Dolag, H Dole, S Donzelli, O Dor??, M Douspis, A Ducout, J Dunkley, X Dupac, G Efstathiou, F Elsner, T A En??lin, H K Eriksen, E Falgarone, F Finelli, O Forni, M Frailis, A A Fraisse, E Franceschi, A Frejsel, S Galeotta, S Galli, K Ganga, T Ghosh, M Giard, Y Giraud-H??raud, E Gjerl??w, J Gonz??lez-Nuevo, K M G??rski, S Gratton, A Gregorio, A Gruppuso, V Guillet, F K Hansen, D Hanson, D L Harrison, G Helou, S Henrot-Versill??, C Hern??ndez-Monteagudo, D Herranz, E Hivon, M Hobson, W A Holmes, K M Huffenberger, G Hurier, A H Jaffe, T R Jaffe, J Jewell, W C Jones, M Juvela, E Keih??nen, R Keskitalo, T S Kisner, R Kneissl, J Knoche, L Knox, N Krachmalnicoff, M Kunz, H Kurki-Suonio, G Lagache, J-M Lamarre, A Lasenby, M Lattanzi, C R Lawrence, J P Leahy, R Leonardi, J Lesgourgues, F Levrier, M Liguori, P B Lilje, M Linden-V??rnle, M L??pez-Caniego, P M Lubin, J F Mac??as-P??rez, B Maffei, D Maino, N Mandolesi, A Mangilli, M Maris, P G Martin, E Mart??nez-Gonz??lez, S Masi, S Matarrese, P Mazzotta, A Melchiorri, L Mendes, A Mennella, M Migliaccio, S Mitra, M-A Miville-Desch??nes, A Moneti, L Montier, G Morgante, D Mortlock, A Moss, D Munshi, J A Murphy, P Naselsky, F Nati, P Natoli, C B Netterfield, H U N??rgaard-Nielsen, F Noviello, D Novikov, I Novikov, L Pagano, F Pajot, R Paladini, D Paoletti, B Partridge, F Pasian, G Patanchon, T J Pearson, O Perdereau, L Perotto, F Perrotta, V Pettorino, F Piacentini, M Piat, E Pierpaoli, D Pietrobon, S Plaszczynski, E Pointecouteau, G Polenta, N Ponthieu, L Popa, G W Pratt, S Prunet, J-L Puget, J P Rachen, W T Reach, R Rebolo, M Remazeilles, C Renault, A Renzi, S Ricciardi, I Ristorcelli, G Rocha, C Rosset, M Rossetti, G Roudier, B Rouill?? d'Orfeuil, J A Rubi??o-Mart??n, B Rusholme, M Sandri, D Santos, M Savelainen, G Savini, D Scott, J D Soler, L D Spencer, V Stolyarov, R Stompor, R Sudiwala, R Sunyaev, D Sutton, A-S Suur-Uski, J-F Sygnet, J A Tauber, L Terenzi, L Toffolatti, M Tomasi, M Tristram, M Tucci, J Tuovinen, L Valenziano, J Valiviita, B Van Tent, L Vibert, P Vielva, F Villa, L A Wade, B D Wandelt, R Watson, I K Wehus, M White, S D M White, D Yvon, A Zacchei, A Zonca

Research output: Contribution to journal › Article › peer-review

88 Downloads (Pure)

Abstract

The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwavebackground ({CMB}) at frequencies above 100GHz. We exploit the Planck {HFI}polarization data from 100 to 353GHz to measure the dust angular powerspectra \$C\_{\textbackslash}ell{\textasciicircum}\{{EE},{BB}\}\$ over the range \$40{\textless}{\textbackslash}ell{\textless}600\$ well awayfrom the Galactic plane. These will bring new insights into interstellardust physics and a precise determination of the level of contaminationfor {CMB} polarization experiments. We show that statistical properties ofthe emission can be characterized over large fractions of the sky using\$C\_{\textbackslash}ell\$. For the dust, they are well described by power laws in \${\textbackslash}ell\$with exponents \${\textbackslash}alpha{\textasciicircum}\{{EE},{BB}\}=-2.42{\textbackslash}pm0.02\$. The amplitudes of thepolarization \$C\_{\textbackslash}ell\$ vary with the average brightness in a way similarto the intensity ones. The dust polarization frequency dependence isconsistent with modified blackbody emission with \${\textbackslash}beta\_d=1.59\$ and\$T\_d=19.6\$K. We find a systematic ratio between the amplitudes of theGalactic \$B\$- and \$E\$-modes of 0.5. We show that even in the faintestdust-emitting regions there are no "clean" windows where primordial {CMB}\$B\$-mode polarization could be measured without subtraction of dustemission. Finally, we investigate the level of dust polarization in the{BICEP}2 experiment field. Extrapolation of the Planck 353GHz data to150GHz gives a dust power \${\textbackslash}ell({\textbackslash}ell+1)C\_{\textbackslash}ell{\textasciicircum}\{{BB}\}/(2{\textbackslash}pi)\$ of\$1.32{\textbackslash}times10{\textasciicircum}\{-2\}{\textbackslash}mu\$K\$\_\{{CMB}\}{\textasciicircum}2\$ over the \$40{\textless}{\textbackslash}ell{\textless}120\$ range;the statistical uncertainty is \${\textbackslash}pm0.29\$ and there is an additionaluncertainty (+0.28,-0.24) from the extrapolation, both in the sameunits. This is the same magnitude as reported by {BICEP}2 over this \${\textbackslash}ell\$range, which highlights the need for assessment of the polarized dustsignal even in the cleanest windows of the sky.

Original language	English
Article number	A133
Journal	Astronomy & Astrophysics
Volume	586
DOIs	https://doi.org/10.1051/0004-6361/201425034
Publication status	Published - Sept 2014

Keywords

Astrophysics - Cosmology and Nongalactic Astrophysics

Access to Document

10.1051/0004-6361/201425034

1

http://adsabs.harvard.edu/abs/2014arXiv1409.5738P

Cite this

Collaboration, P., 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-L??vy, A., Bernard, J-P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., ... Zonca, A. (2014). Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes. Astronomy & Astrophysics, 586, Article A133. https://doi.org/10.1051/0004-6361/201425034

@article{4b03ea5e68a1412d92debe35eb1e8b5b,

title = "Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes",

abstract = "The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwavebackground ({CMB}) at frequencies above 100GHz. We exploit the Planck {HFI}polarization data from 100 to 353GHz to measure the dust angular powerspectra \$C\_{\textbackslash}ell{\textasciicircum}\{{EE},{BB}\}\$ over the range \$40{\textless}{\textbackslash}ell{\textless}600\$ well awayfrom the Galactic plane. These will bring new insights into interstellardust physics and a precise determination of the level of contaminationfor {CMB} polarization experiments. We show that statistical properties ofthe emission can be characterized over large fractions of the sky using\$C\_{\textbackslash}ell\$. For the dust, they are well described by power laws in \${\textbackslash}ell\$with exponents \${\textbackslash}alpha{\textasciicircum}\{{EE},{BB}\}=-2.42{\textbackslash}pm0.02\$. The amplitudes of thepolarization \$C\_{\textbackslash}ell\$ vary with the average brightness in a way similarto the intensity ones. The dust polarization frequency dependence isconsistent with modified blackbody emission with \${\textbackslash}beta\_d=1.59\$ and\$T\_d=19.6\$K. We find a systematic ratio between the amplitudes of theGalactic \$B\$- and \$E\$-modes of 0.5. We show that even in the faintestdust-emitting regions there are no {"}clean{"} windows where primordial {CMB}\$B\$-mode polarization could be measured without subtraction of dustemission. Finally, we investigate the level of dust polarization in the{BICEP}2 experiment field. Extrapolation of the Planck 353GHz data to150GHz gives a dust power \${\textbackslash}ell({\textbackslash}ell+1)C\_{\textbackslash}ell{\textasciicircum}\{{BB}\}/(2{\textbackslash}pi)\$ of\$1.32{\textbackslash}times10{\textasciicircum}\{-2\}{\textbackslash}mu\$K\$\_\{{CMB}\}{\textasciicircum}2\$ over the \$40{\textless}{\textbackslash}ell{\textless}120\$ range;the statistical uncertainty is \${\textbackslash}pm0.29\$ and there is an additionaluncertainty (+0.28,-0.24) from the extrapolation, both in the sameunits. This is the same magnitude as reported by {BICEP}2 over this \${\textbackslash}ell\$range, which highlights the need for assessment of the polarized dustsignal even in the cleanest windows of the sky.",

keywords = "Astrophysics - Cosmology and Nongalactic Astrophysics",

author = "Planck Collaboration and R Adam and Ade, {P A R} and N Aghanim and M Arnaud and J Aumont and C Baccigalupi and Banday, {A J} and Barreiro, {R B} and Bartlett, {J G} and N Bartolo and E Battaner and K Benabed and A Benoit-L??vy and J-P Bernard and M Bersanelli and P Bielewicz and A Bonaldi and L Bonavera and Bond, {J R} and J Borrill and Bouchet, {F R} and F Boulanger and A Bracco and M Bucher and C Burigana and Butler, {R C} and E Calabrese and J-F Cardoso and A Catalano and A Challinor and A Chamballu and R-R Chary and Chiang, {H C} and Christensen, {P R} and Clements, {D L} and S Colombi and Colombo, {L P L} and C Combet and F Couchot and A Coulais and Crill, {B P} and A Curto and F Cuttaia and L Danese and Davies, {R D} and Davis, {R J} and {de Bernardis}, P and {de Zotti}, G and J Delabrouille and J-M Delouis and F-X D??sert and C Dickinson and Diego, {J M} and K Dolag and H Dole and S Donzelli and O Dor?? and M Douspis and A Ducout and J Dunkley and X Dupac and G Efstathiou and F Elsner and En??lin, {T A} and Eriksen, {H K} and E Falgarone and F Finelli and O Forni and M Frailis and Fraisse, {A A} and E Franceschi and A Frejsel and S Galeotta and S Galli and K Ganga and T Ghosh and M Giard and Y Giraud-H??raud and E Gjerl??w and J Gonz??lez-Nuevo and G??rski, {K M} and S Gratton and A Gregorio and A Gruppuso and V Guillet and Hansen, {F K} and D Hanson and Harrison, {D L} and G Helou and S Henrot-Versill?? and C Hern??ndez-Monteagudo and D Herranz and E Hivon and M Hobson and Holmes, {W A} and Huffenberger, {K M} and G Hurier and Jaffe, {A H} and Jaffe, {T R} and J Jewell and Jones, {W C} and M Juvela and E Keih??nen and R Keskitalo and Kisner, {T S} and R Kneissl and J Knoche and L Knox and N Krachmalnicoff and M Kunz and H Kurki-Suonio and G Lagache and J-M Lamarre and A Lasenby and M Lattanzi and Lawrence, {C R} and Leahy, {J P} and R Leonardi and J Lesgourgues and F Levrier and M Liguori and Lilje, {P B} and M Linden-V??rnle and M L??pez-Caniego and Lubin, {P M} and Mac??as-P??rez, {J F} and B Maffei and D Maino and N Mandolesi and A Mangilli and M Maris and Martin, {P G} and E Mart??nez-Gonz??lez and S Masi and S Matarrese and P Mazzotta and A Melchiorri and L Mendes and A Mennella and M Migliaccio and S Mitra and M-A Miville-Desch??nes and A Moneti and L Montier and G Morgante and D Mortlock and A Moss and D Munshi and Murphy, {J A} and P Naselsky and F Nati and P Natoli and Netterfield, {C B} and N??rgaard-Nielsen, {H U} and F Noviello and D Novikov and I Novikov and L Pagano and F Pajot and R Paladini and D Paoletti and B Partridge and F Pasian and G Patanchon and Pearson, {T J} and O Perdereau and L Perotto and F Perrotta and V Pettorino and F Piacentini and M Piat and E Pierpaoli and D Pietrobon and S Plaszczynski and E Pointecouteau and G Polenta and N Ponthieu and L Popa and Pratt, {G W} and S Prunet and J-L Puget and Rachen, {J P} and Reach, {W T} and R Rebolo and M Remazeilles and C Renault and A Renzi and S Ricciardi and I Ristorcelli and G Rocha and C Rosset and M Rossetti and G Roudier and {Rouill?? d'Orfeuil}, B and Rubi??o-Mart??n, {J A} and B Rusholme and M Sandri and D Santos and M Savelainen and G Savini and D Scott and Soler, {J D} and Spencer, {L D} and V Stolyarov and R Stompor and R Sudiwala and R Sunyaev and D Sutton and A-S Suur-Uski and J-F Sygnet and Tauber, {J A} and L Terenzi and L Toffolatti and M Tomasi and M Tristram and M Tucci and J Tuovinen and L Valenziano and J Valiviita and {Van Tent}, B and L Vibert and P Vielva and F Villa and Wade, {L A} and Wandelt, {B D} and R Watson and Wehus, {I K} and M White and White, {S D M} and D Yvon and A Zacchei and A Zonca",

year = "2014",

month = sep,

doi = "10.1051/0004-6361/201425034",

language = "English",

volume = "586",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Collaboration, P, Adam, R, Ade, PAR, Aghanim, N, Arnaud, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartlett, JG, Bartolo, N, Battaner, E, Benabed, K, Benoit-L??vy, A, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, J-F, Catalano, A, Challinor, A, Chamballu, A, Chary, R-R, Chiang, HC, Christensen, PR, Clements, DL, Colombi, S, Colombo, LPL, Combet, C, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, de Bernardis, P, de Zotti, G, Delabrouille, J, Delouis, J-M, D??sert, F-X, Dickinson, C, Diego, JM, Dolag, K, Dole, H, Donzelli, S, Dor??, O, Douspis, M, Ducout, A, Dunkley, J, Dupac, X, Efstathiou, G, Elsner, F, En??lin, TA, Eriksen, HK, Falgarone, E, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Giraud-H??raud, Y, Gjerl??w, E, Gonz??lez-Nuevo, J, G??rski, KM, Gratton, S, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, FK, Hanson, D, Harrison, DL, Helou, G, Henrot-Versill??, S, Hern??ndez-Monteagudo, C, Herranz, D, Hivon, E, Hobson, M, Holmes, WA, Huffenberger, KM, Hurier, G, Jaffe, AH, Jaffe, TR, Jewell, J, Jones, WC, Juvela, M, Keih??nen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Knox, L, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Leahy, JP, Leonardi, R, Lesgourgues, J, Levrier, F, Liguori, M, Lilje, PB, Linden-V??rnle, M, L??pez-Caniego, M, Lubin, PM, Mac??as-P??rez, JF, Maffei, B, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, PG, Mart??nez-Gonz??lez, E, Masi, S, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville-Desch??nes, M-A, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Moss, A, Munshi, D, Murphy, JA, Naselsky, P, Nati, F, Natoli, P, Netterfield, CB, N??rgaard-Nielsen, HU, Noviello, F, Novikov, D, Novikov, I, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Pearson, TJ, 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, GW, Prunet, S, Puget, J-L, Rachen, JP, Reach, WT, Rebolo, R, Remazeilles, M, Renault, C, Renzi, A, Ricciardi, S, Ristorcelli, I, Rocha, G, Rosset, C, Rossetti, M, Roudier, G, Rouill?? d'Orfeuil, B, Rubi??o-Mart??n, JA, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Savini, G, Scott, D, Soler, JD, Spencer, LD, Stolyarov, V, Stompor, R, Sudiwala, R, Sunyaev, R, Sutton, D, Suur-Uski, A-S, Sygnet, J-F, Tauber, JA, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Valenziano, L, Valiviita, J, Van Tent, B, Vibert, L, Vielva, P, Villa, F, Wade, LA, Wandelt, BD, Watson, R, Wehus, IK, White, M, White, SDM, Yvon, D, Zacchei, A & Zonca, A 2014, 'Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes', Astronomy & Astrophysics, vol. 586, A133. https://doi.org/10.1051/0004-6361/201425034

TY - JOUR

T1 - Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes

AU - Collaboration, Planck

AU - Adam, R

AU - Ade, P A R

AU - Aghanim, N

AU - Arnaud, M

AU - Aumont, J

AU - Baccigalupi, C

AU - Banday, A J

AU - Barreiro, R B

AU - Bartlett, J G

AU - Bartolo, N

AU - Battaner, E

AU - Benabed, K

AU - Benoit-L??vy, A

AU - Bernard, J-P

AU - Bersanelli, M

AU - Bielewicz, P

AU - Bonaldi, A

AU - Bonavera, L

AU - Bond, J R

AU - Borrill, J

AU - Bouchet, F R

AU - Boulanger, F

AU - Bracco, A

AU - Bucher, M

AU - Burigana, C

AU - Butler, R C

AU - Calabrese, E

AU - Cardoso, J-F

AU - Catalano, A

AU - Challinor, A

AU - Chamballu, A

AU - Chary, R-R

AU - Chiang, H C

AU - Christensen, P R

AU - Clements, D L

AU - Colombi, S

AU - Colombo, L P L

AU - Combet, C

AU - Couchot, F

AU - Coulais, A

AU - Crill, B P

AU - Curto, A

AU - Cuttaia, F

AU - Danese, L

AU - Davies, R D

AU - Davis, R J

AU - de Bernardis, P

AU - de Zotti, G

AU - Delabrouille, J

AU - Delouis, J-M

AU - D??sert, F-X

AU - Dickinson, C

AU - Diego, J M

AU - Dolag, K

AU - Dole, H

AU - Donzelli, S

AU - Dor??, O

AU - Douspis, M

AU - Ducout, A

AU - Dunkley, J

AU - Dupac, X

AU - Efstathiou, G

AU - Elsner, F

AU - En??lin, T A

AU - Eriksen, H K

AU - Falgarone, E

AU - Finelli, F

AU - Forni, O

AU - Frailis, M

AU - Fraisse, A A

AU - Franceschi, E

AU - Frejsel, A

AU - Galeotta, S

AU - Galli, S

AU - Ganga, K

AU - Ghosh, T

AU - Giard, M

AU - Giraud-H??raud, Y

AU - Gjerl??w, E

AU - Gonz??lez-Nuevo, J

AU - G??rski, K M

AU - Gratton, S

AU - Gregorio, A

AU - Gruppuso, A

AU - Guillet, V

AU - Hansen, F K

AU - Hanson, D

AU - Harrison, D L

AU - Helou, G

AU - Henrot-Versill??, S

AU - Hern??ndez-Monteagudo, C

AU - Herranz, D

AU - Hivon, E

AU - Hobson, M

AU - Holmes, W A

AU - Huffenberger, K M

AU - Hurier, G

AU - Jaffe, A H

AU - Jaffe, T R

AU - Jewell, J

AU - Jones, W C

AU - Juvela, M

AU - Keih??nen, E

AU - Keskitalo, R

AU - Kisner, T S

AU - Kneissl, R

AU - Knoche, J

AU - Knox, L

AU - Krachmalnicoff, N

AU - Kunz, M

AU - Kurki-Suonio, H

AU - Lagache, G

AU - Lamarre, J-M

AU - Lasenby, A

AU - Lattanzi, M

AU - Lawrence, C R

AU - Leahy, J P

AU - Leonardi, R

AU - Lesgourgues, J

AU - Levrier, F

AU - Liguori, M

AU - Lilje, P B

AU - Linden-V??rnle, M

AU - L??pez-Caniego, M

AU - Lubin, P M

AU - Mac??as-P??rez, J F

AU - Maffei, B

AU - Maino, D

AU - Mandolesi, N

AU - Mangilli, A

AU - Maris, M

AU - Martin, P G

AU - Mart??nez-Gonz??lez, E

AU - Masi, S

AU - Matarrese, S

AU - Mazzotta, P

AU - Melchiorri, A

AU - Mendes, L

AU - Mennella, A

AU - Migliaccio, M

AU - Mitra, S

AU - Miville-Desch??nes, M-A

AU - Moneti, A

AU - Montier, L

AU - Morgante, G

AU - Mortlock, D

AU - Moss, A

AU - Munshi, D

AU - Murphy, J A

AU - Naselsky, P

AU - Nati, F

AU - Natoli, P

AU - Netterfield, C B

AU - N??rgaard-Nielsen, H U

AU - Noviello, F

AU - Novikov, D

AU - Novikov, I

AU - Pagano, L

AU - Pajot, F

AU - Paladini, R

AU - Paoletti, D

AU - Partridge, B

AU - Pasian, F

AU - Patanchon, G

AU - Pearson, T J

AU - Perdereau, O

AU - Perotto, L

AU - Perrotta, F

AU - Pettorino, V

AU - Piacentini, F

AU - Piat, M

AU - Pierpaoli, E

AU - Pietrobon, D

AU - Plaszczynski, S

AU - Pointecouteau, E

AU - Polenta, G

AU - Ponthieu, N

AU - Popa, L

AU - Pratt, G W

AU - Prunet, S

AU - Puget, J-L

AU - Rachen, J P

AU - Reach, W T

AU - Rebolo, R

AU - Remazeilles, M

AU - Renault, C

AU - Renzi, A

AU - Ricciardi, S

AU - Ristorcelli, I

AU - Rocha, G

AU - Rosset, C

AU - Rossetti, M

AU - Roudier, G

AU - Rouill?? d'Orfeuil, B

AU - Rubi??o-Mart??n, J A

AU - Rusholme, B

AU - Sandri, M

AU - Santos, D

AU - Savelainen, M

AU - Savini, G

AU - Scott, D

AU - Soler, J D

AU - Spencer, L D

AU - Stolyarov, V

AU - Stompor, R

AU - Sudiwala, R

AU - Sunyaev, R

AU - Sutton, D

AU - Suur-Uski, A-S

AU - Sygnet, J-F

AU - Tauber, J A

AU - Terenzi, L

AU - Toffolatti, L

AU - Tomasi, M

AU - Tristram, M

AU - Tucci, M

AU - Tuovinen, J

AU - Valenziano, L

AU - Valiviita, J

AU - Van Tent, B

AU - Vibert, L

AU - Vielva, P

AU - Villa, F

AU - Wade, L A

AU - Wandelt, B D

AU - Watson, R

AU - Wehus, I K

AU - White, M

AU - White, S D M

AU - Yvon, D

AU - Zacchei, A

AU - Zonca, A

PY - 2014/9

Y1 - 2014/9

N2 - The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwavebackground ({CMB}) at frequencies above 100GHz. We exploit the Planck {HFI}polarization data from 100 to 353GHz to measure the dust angular powerspectra \$C\_{\textbackslash}ell{\textasciicircum}\{{EE},{BB}\}\$ over the range \$40{\textless}{\textbackslash}ell{\textless}600\$ well awayfrom the Galactic plane. These will bring new insights into interstellardust physics and a precise determination of the level of contaminationfor {CMB} polarization experiments. We show that statistical properties ofthe emission can be characterized over large fractions of the sky using\$C\_{\textbackslash}ell\$. For the dust, they are well described by power laws in \${\textbackslash}ell\$with exponents \${\textbackslash}alpha{\textasciicircum}\{{EE},{BB}\}=-2.42{\textbackslash}pm0.02\$. The amplitudes of thepolarization \$C\_{\textbackslash}ell\$ vary with the average brightness in a way similarto the intensity ones. The dust polarization frequency dependence isconsistent with modified blackbody emission with \${\textbackslash}beta\_d=1.59\$ and\$T\_d=19.6\$K. We find a systematic ratio between the amplitudes of theGalactic \$B\$- and \$E\$-modes of 0.5. We show that even in the faintestdust-emitting regions there are no "clean" windows where primordial {CMB}\$B\$-mode polarization could be measured without subtraction of dustemission. Finally, we investigate the level of dust polarization in the{BICEP}2 experiment field. Extrapolation of the Planck 353GHz data to150GHz gives a dust power \${\textbackslash}ell({\textbackslash}ell+1)C\_{\textbackslash}ell{\textasciicircum}\{{BB}\}/(2{\textbackslash}pi)\$ of\$1.32{\textbackslash}times10{\textasciicircum}\{-2\}{\textbackslash}mu\$K\$\_\{{CMB}\}{\textasciicircum}2\$ over the \$40{\textless}{\textbackslash}ell{\textless}120\$ range;the statistical uncertainty is \${\textbackslash}pm0.29\$ and there is an additionaluncertainty (+0.28,-0.24) from the extrapolation, both in the sameunits. This is the same magnitude as reported by {BICEP}2 over this \${\textbackslash}ell\$range, which highlights the need for assessment of the polarized dustsignal even in the cleanest windows of the sky.

AB - The polarized thermal emission from Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwavebackground ({CMB}) at frequencies above 100GHz. We exploit the Planck {HFI}polarization data from 100 to 353GHz to measure the dust angular powerspectra \$C\_{\textbackslash}ell{\textasciicircum}\{{EE},{BB}\}\$ over the range \$40{\textless}{\textbackslash}ell{\textless}600\$ well awayfrom the Galactic plane. These will bring new insights into interstellardust physics and a precise determination of the level of contaminationfor {CMB} polarization experiments. We show that statistical properties ofthe emission can be characterized over large fractions of the sky using\$C\_{\textbackslash}ell\$. For the dust, they are well described by power laws in \${\textbackslash}ell\$with exponents \${\textbackslash}alpha{\textasciicircum}\{{EE},{BB}\}=-2.42{\textbackslash}pm0.02\$. The amplitudes of thepolarization \$C\_{\textbackslash}ell\$ vary with the average brightness in a way similarto the intensity ones. The dust polarization frequency dependence isconsistent with modified blackbody emission with \${\textbackslash}beta\_d=1.59\$ and\$T\_d=19.6\$K. We find a systematic ratio between the amplitudes of theGalactic \$B\$- and \$E\$-modes of 0.5. We show that even in the faintestdust-emitting regions there are no "clean" windows where primordial {CMB}\$B\$-mode polarization could be measured without subtraction of dustemission. Finally, we investigate the level of dust polarization in the{BICEP}2 experiment field. Extrapolation of the Planck 353GHz data to150GHz gives a dust power \${\textbackslash}ell({\textbackslash}ell+1)C\_{\textbackslash}ell{\textasciicircum}\{{BB}\}/(2{\textbackslash}pi)\$ of\$1.32{\textbackslash}times10{\textasciicircum}\{-2\}{\textbackslash}mu\$K\$\_\{{CMB}\}{\textasciicircum}2\$ over the \$40{\textless}{\textbackslash}ell{\textless}120\$ range;the statistical uncertainty is \${\textbackslash}pm0.29\$ and there is an additionaluncertainty (+0.28,-0.24) from the extrapolation, both in the sameunits. This is the same magnitude as reported by {BICEP}2 over this \${\textbackslash}ell\$range, which highlights the need for assessment of the polarized dustsignal even in the cleanest windows of the sky.

KW - Astrophysics - Cosmology and Nongalactic Astrophysics

U2 - 10.1051/0004-6361/201425034

DO - 10.1051/0004-6361/201425034

M3 - Article

SN - 0004-6361

VL - 586

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A133

ER -

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

Abstract

Keywords

Access to Document

Fingerprint

Cite this