Abstract
The polarized thermal emission from diffuse Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100 GHz. In this paper we exploit the uniqueness of the Planck HFI polarization data from 100 to 353 GHz to measure the polarized dust angular power spectra CℓEE and CℓBB over the multipole range 40 < ℓ < 600 well away from the Galactic plane. These measurements will bring new insights into interstellar dust physics and allow a precise determination of the level of contamination for CMB polarization experiments. Despite the non-Gaussian and anisotropic nature of Galactic dust, we show that general statistical properties of the emission can be characterized accurately over large fractions of the sky using angular power spectra. The polarization power spectra of the dust are well described by power laws in multipole, Cℓ ∝ ℓα, with exponents αEE,BB = -2.42 ± 0.02. The amplitudes of the polarization power spectra vary with the average brightness in a way similar to the intensity power spectra. The frequency dependence of the dust polarization spectra is consistent with modified blackbody emission with βd = 1.59 and Td = 19.6 K down to the lowest Planck HFI frequencies. We find a systematic difference between the amplitudes of the Galactic B- and E-modes, CℓBB/CℓEE = 0.5. We verify that these general properties are preserved towards high Galactic latitudes with low dust column densities. We show that even in the faintest dust-emitting regions there are no "clean" windows in the sky where primordial CMB B-mode polarization measurements could be made without subtraction of foreground emission. Finally, we investigate the level of dust polarization in the specific field recently targeted by the BICEP2 experiment. Extrapolation of the Planck 353 GHz data to 150 GHz gives a dust power DℓBB ≡ ℓ(ℓ +1)CℓBB/(2π) of 1.32 × 10-2 μKCMB2 over the multipole range of the primordial recombination bump (40 < ℓ < 120); the statistical uncertainty is ± 0.29 × 10-2 μKCMB2 and there is an additional uncertainty (+0.28, -0.24) × 10-2 μKCMB2 from the extrapolation. This level is the same magnitude as reported by BICEP2 over this ℓ range, which highlights the need for assessment of the polarized dust signal even in the cleanest windows of the sky.
| Original language | English (US) |
|---|---|
| Article number | A133 |
| Journal | Astronomy and Astrophysics |
| Volume | 586 |
| DOIs | |
| State | Published - Feb 1 2016 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Keywords
- ISM: magnetic fields
- ISM: structure
- cosmic background radiation
- cosmology: observations
- polarization
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Planck intermediate results : XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes. / 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-Lévy, 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.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; De Bernardis, P.; De Zotti, G.; Delabrouille, J.; Delouis, J. M.; Désert, F. X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, 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-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hivon, E.; Hobson, M.; Holmes, W. A.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jewell, J.; Jones, W. C.; Juvela, M.; Keihänen, 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-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Mangilli, A.; Maris, M.; Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, 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.; Nørgaard-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.; Rouillé D'Orfeuil, B.; Rubiño-Martín, 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.; Toffolatti, 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.
In: Astronomy and Astrophysics, Vol. 586, A133, 01.02.2016.Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - Planck intermediate results
T2 - XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes
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-Lévy, 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 - Désert, F. X.
AU - Dickinson, C.
AU - Diego, J. M.
AU - Dolag, K.
AU - Dole, H.
AU - Donzelli, S.
AU - Doré, O.
AU - Douspis, M.
AU - Ducout, A.
AU - Dunkley, J.
AU - Dupac, X.
AU - Efstathiou, G.
AU - Elsner, F.
AU - Enßlin, 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-Héraud, Y.
AU - Gjerløw, E.
AU - González-Nuevo, J.
AU - Górski, 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-Versillé, S.
AU - Hernández-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 - Keihänen, 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-Vørnle, M.
AU - López-Caniego, M.
AU - Lubin, P. M.
AU - Macías-Pérez, J. F.
AU - Maffei, B.
AU - Maino, D.
AU - Mandolesi, N.
AU - Mangilli, A.
AU - Maris, M.
AU - Martin, P. G.
AU - Martínez-González, E.
AU - Masi, S.
AU - Matarrese, S.
AU - Mazzotta, P.
AU - Meinhold, P. R.
AU - Melchiorri, A.
AU - Mendes, L.
AU - Mennella, A.
AU - Migliaccio, M.
AU - Mitra, S.
AU - Miville-Deschênes, 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 - Nørgaard-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 - Rouillé D'Orfeuil, B.
AU - Rubiño-Martín, 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.
N1 - Funding Information: The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaboration . Some of the results in this paper have been derived using the HEALPix package. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934. Publisher Copyright: © ESO, 2016.
PY - 2016/2/1
Y1 - 2016/2/1
N2 - The polarized thermal emission from diffuse Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100 GHz. In this paper we exploit the uniqueness of the Planck HFI polarization data from 100 to 353 GHz to measure the polarized dust angular power spectra CℓEE and CℓBB over the multipole range 40 < ℓ < 600 well away from the Galactic plane. These measurements will bring new insights into interstellar dust physics and allow a precise determination of the level of contamination for CMB polarization experiments. Despite the non-Gaussian and anisotropic nature of Galactic dust, we show that general statistical properties of the emission can be characterized accurately over large fractions of the sky using angular power spectra. The polarization power spectra of the dust are well described by power laws in multipole, Cℓ ∝ ℓα, with exponents αEE,BB = -2.42 ± 0.02. The amplitudes of the polarization power spectra vary with the average brightness in a way similar to the intensity power spectra. The frequency dependence of the dust polarization spectra is consistent with modified blackbody emission with βd = 1.59 and Td = 19.6 K down to the lowest Planck HFI frequencies. We find a systematic difference between the amplitudes of the Galactic B- and E-modes, CℓBB/CℓEE = 0.5. We verify that these general properties are preserved towards high Galactic latitudes with low dust column densities. We show that even in the faintest dust-emitting regions there are no "clean" windows in the sky where primordial CMB B-mode polarization measurements could be made without subtraction of foreground emission. Finally, we investigate the level of dust polarization in the specific field recently targeted by the BICEP2 experiment. Extrapolation of the Planck 353 GHz data to 150 GHz gives a dust power DℓBB ≡ ℓ(ℓ +1)CℓBB/(2π) of 1.32 × 10-2 μKCMB2 over the multipole range of the primordial recombination bump (40 < ℓ < 120); the statistical uncertainty is ± 0.29 × 10-2 μKCMB2 and there is an additional uncertainty (+0.28, -0.24) × 10-2 μKCMB2 from the extrapolation. This level is the same magnitude as reported by BICEP2 over this ℓ range, which highlights the need for assessment of the polarized dust signal even in the cleanest windows of the sky.
AB - The polarized thermal emission from diffuse Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100 GHz. In this paper we exploit the uniqueness of the Planck HFI polarization data from 100 to 353 GHz to measure the polarized dust angular power spectra CℓEE and CℓBB over the multipole range 40 < ℓ < 600 well away from the Galactic plane. These measurements will bring new insights into interstellar dust physics and allow a precise determination of the level of contamination for CMB polarization experiments. Despite the non-Gaussian and anisotropic nature of Galactic dust, we show that general statistical properties of the emission can be characterized accurately over large fractions of the sky using angular power spectra. The polarization power spectra of the dust are well described by power laws in multipole, Cℓ ∝ ℓα, with exponents αEE,BB = -2.42 ± 0.02. The amplitudes of the polarization power spectra vary with the average brightness in a way similar to the intensity power spectra. The frequency dependence of the dust polarization spectra is consistent with modified blackbody emission with βd = 1.59 and Td = 19.6 K down to the lowest Planck HFI frequencies. We find a systematic difference between the amplitudes of the Galactic B- and E-modes, CℓBB/CℓEE = 0.5. We verify that these general properties are preserved towards high Galactic latitudes with low dust column densities. We show that even in the faintest dust-emitting regions there are no "clean" windows in the sky where primordial CMB B-mode polarization measurements could be made without subtraction of foreground emission. Finally, we investigate the level of dust polarization in the specific field recently targeted by the BICEP2 experiment. Extrapolation of the Planck 353 GHz data to 150 GHz gives a dust power DℓBB ≡ ℓ(ℓ +1)CℓBB/(2π) of 1.32 × 10-2 μKCMB2 over the multipole range of the primordial recombination bump (40 < ℓ < 120); the statistical uncertainty is ± 0.29 × 10-2 μKCMB2 and there is an additional uncertainty (+0.28, -0.24) × 10-2 μKCMB2 from the extrapolation. This level is the same magnitude as reported by BICEP2 over this ℓ range, which highlights the need for assessment of the polarized dust signal even in the cleanest windows of the sky.
KW - ISM: magnetic fields
KW - ISM: structure
KW - cosmic background radiation
KW - cosmology: observations
KW - polarization
UR - http://www.scopus.com/inward/record.url?scp=84958967480&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84958967480&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201425034
DO - 10.1051/0004-6361/201425034
M3 - Article
AN - SCOPUS:84958967480
VL - 586
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A133
ER -