Abstract
The quest for a B-mode imprint from primordial gravity waves on the polarization of the cosmic microwave background (CMB) requires the characterization of foreground polarization from Galactic dust. We present a statistical study of the filamentary structure of the 353 GHz Planck Stokes maps at high Galactic latitude, relevant to the study of dust emission as a polarized foreground to the CMB. We filter the intensity and polarization maps to isolate filaments in the range of angular scales where the power asymmetry between E-modes and B-modes is observed. Using the Smoothed Hessian Major Axis Filament Finder (SMAFF), we identify 259 filaments at high Galactic latitude, with lengths larger or equal to 2° (corresponding to 3.5 pc in length for a typical distance of 100 pc). These filaments show a preferred orientation parallel to the magnetic field projected onto the plane of the sky, derived from their polarization angles. We present mean maps of the filaments in Stokes I, Q, U, E, and B, computed by stacking individual images rotated to align the orientations of the filaments. Combining the stacked images and the histogram of relative orientations, we estimate the mean polarization fraction of the filaments to be 11%. Furthermore, we show that the correlation between the filaments and the magnetic field orientations may account for the E and B asymmetry and the CℓTE/CℓEE ratio, reported in the power spectra analysis of the Planck353 GHz polarization maps. Future models of the dust foreground for CMB polarization studies will need to take into account the observed correlation between the dust polarization and the structure of interstellar matter.
| Original language | English (US) |
|---|---|
| Article number | A141 |
| 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
- Galaxies: ISM
- ISM: general
- Polarization
- Submillimeter: ISM
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Planck intermediate results : XXXVIII. E- and B-modes of dust polarization from the magnetized filamentary structure of the interstellar medium. / Ade, P. A.R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; 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.; Burigana, C.; Calabrese, E.; Cardoso, J. F.; Catalano, A.; Chamballu, A.; Chary, R. R.; Chiang, H. C.; Christensen, P. R.; Colombo, L. P.L.; Combet, C.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; De Bernardis, P.; De Rosa, A.; De Zotti, G.; Delabrouille, J.; Delouis, J. M.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Ferrière, K.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frolov, A.; Galeotta, S.; Galli, S.; Ganga, K.; Ghosh, T.; Giard, M.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Harrison, D. L.; Helou, G.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hornstrup, A.; Hovest, W.; Huang, Z.; Huffenberger, K. M.; Hurier, G.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lamarre, J. M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; León-Tavares, 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.; Maris, M.; Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; McGehee, P.; Melchiorri, A.; Mennella, A.; Migliaccio, M.; Miville-Deschênes, M. A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Novikov, D.; Novikov, I.; Oppermann, N.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Perdereau, O.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Pratt, G. W.; Prunet, S.; Puget, J. L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Savini, G.; Scott, D.; Serra, P.; Soler, J. D.; Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Suur-Uski, A. S.; Sygnet, J. F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Yvon, D.; Zacchei, A.; Zonca, A.
In: Astronomy and Astrophysics, Vol. 586, A141, 01.02.2016.Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - Planck intermediate results
T2 - XXXVIII. E- and B-modes of dust polarization from the magnetized filamentary structure of the interstellar medium
AU - Ade, P. A.R.
AU - Aghanim, N.
AU - Arnaud, M.
AU - Ashdown, M.
AU - Aumont, J.
AU - Baccigalupi, C.
AU - Banday, A. J.
AU - Barreiro, R. B.
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 - Burigana, C.
AU - Calabrese, E.
AU - Cardoso, J. F.
AU - Catalano, A.
AU - Chamballu, A.
AU - Chary, R. R.
AU - Chiang, H. C.
AU - Christensen, P. R.
AU - Colombo, L. P.L.
AU - Combet, C.
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 Rosa, A.
AU - De Zotti, G.
AU - Delabrouille, J.
AU - Delouis, J. M.
AU - Dickinson, C.
AU - Diego, J. M.
AU - Dole, H.
AU - Donzelli, S.
AU - Doré, O.
AU - Douspis, M.
AU - Dunkley, J.
AU - Dupac, X.
AU - Efstathiou, G.
AU - Elsner, F.
AU - Enßlin, T. A.
AU - Eriksen, H. K.
AU - Falgarone, E.
AU - Ferrière, K.
AU - Finelli, F.
AU - Forni, O.
AU - Frailis, M.
AU - Fraisse, A. A.
AU - Franceschi, E.
AU - Frolov, A.
AU - Galeotta, S.
AU - Galli, S.
AU - Ganga, K.
AU - Ghosh, T.
AU - Giard, M.
AU - Gjerløw, E.
AU - González-Nuevo, J.
AU - Górski, K. M.
AU - Gruppuso, A.
AU - Guillet, V.
AU - Hansen, F. K.
AU - Harrison, D. L.
AU - Helou, G.
AU - Hernández-Monteagudo, C.
AU - Herranz, D.
AU - Hildebrandt, S. R.
AU - Hivon, E.
AU - Hornstrup, A.
AU - Hovest, W.
AU - Huang, Z.
AU - Huffenberger, K. M.
AU - Hurier, G.
AU - Jaffe, T. R.
AU - Jones, W. C.
AU - Juvela, M.
AU - Keihänen, E.
AU - Keskitalo, R.
AU - Kisner, T. S.
AU - Kneissl, R.
AU - Knoche, J.
AU - Kunz, M.
AU - Kurki-Suonio, H.
AU - Lamarre, J. M.
AU - Lasenby, A.
AU - Lattanzi, M.
AU - Lawrence, C. R.
AU - Leonardi, R.
AU - León-Tavares, 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 - Maris, M.
AU - Martin, P. G.
AU - Martínez-González, E.
AU - Masi, S.
AU - Matarrese, S.
AU - McGehee, P.
AU - Melchiorri, A.
AU - Mennella, A.
AU - Migliaccio, M.
AU - Miville-Deschênes, M. A.
AU - Moneti, A.
AU - Montier, L.
AU - Morgante, G.
AU - Mortlock, D.
AU - Munshi, D.
AU - Murphy, J. A.
AU - Naselsky, P.
AU - Nati, F.
AU - Natoli, P.
AU - Novikov, D.
AU - Novikov, I.
AU - Oppermann, N.
AU - Oxborrow, C. A.
AU - Pagano, L.
AU - Pajot, F.
AU - Paoletti, D.
AU - Pasian, F.
AU - Perdereau, O.
AU - Pettorino, V.
AU - Piacentini, F.
AU - Piat, M.
AU - Pierpaoli, E.
AU - Plaszczynski, S.
AU - Pointecouteau, E.
AU - Polenta, G.
AU - Ponthieu, N.
AU - Pratt, G. W.
AU - Prunet, S.
AU - Puget, J. L.
AU - Rachen, J. P.
AU - Reach, W. T.
AU - Rebolo, R.
AU - Reinecke, M.
AU - Remazeilles, M.
AU - Renault, C.
AU - Renzi, A.
AU - Ristorcelli, I.
AU - Rocha, G.
AU - Rosset, C.
AU - Rossetti, M.
AU - Roudier, G.
AU - Rubiño-Martín, J. A.
AU - Rusholme, B.
AU - Sandri, M.
AU - Santos, D.
AU - Savelainen, M.
AU - Savini, G.
AU - Scott, D.
AU - Serra, P.
AU - Soler, J. D.
AU - Stolyarov, V.
AU - Sudiwala, R.
AU - Sunyaev, R.
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 - Umana, G.
AU - Valenziano, L.
AU - Valiviita, J.
AU - Van Tent, B.
AU - Vielva, P.
AU - Villa, F.
AU - Wade, L. A.
AU - Wandelt, B. D.
AU - Wehus, I. K.
AU - Yvon, D.
AU - Zacchei, A.
AU - Zonca, A.
N1 - Funding Information: The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA 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); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration . The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/20072013)/ERC grant agreement No. 267934. Some of the results in this paper have been derived using the package. Publisher Copyright: © ESO, 2016.
PY - 2016/2/1
Y1 - 2016/2/1
N2 - The quest for a B-mode imprint from primordial gravity waves on the polarization of the cosmic microwave background (CMB) requires the characterization of foreground polarization from Galactic dust. We present a statistical study of the filamentary structure of the 353 GHz Planck Stokes maps at high Galactic latitude, relevant to the study of dust emission as a polarized foreground to the CMB. We filter the intensity and polarization maps to isolate filaments in the range of angular scales where the power asymmetry between E-modes and B-modes is observed. Using the Smoothed Hessian Major Axis Filament Finder (SMAFF), we identify 259 filaments at high Galactic latitude, with lengths larger or equal to 2° (corresponding to 3.5 pc in length for a typical distance of 100 pc). These filaments show a preferred orientation parallel to the magnetic field projected onto the plane of the sky, derived from their polarization angles. We present mean maps of the filaments in Stokes I, Q, U, E, and B, computed by stacking individual images rotated to align the orientations of the filaments. Combining the stacked images and the histogram of relative orientations, we estimate the mean polarization fraction of the filaments to be 11%. Furthermore, we show that the correlation between the filaments and the magnetic field orientations may account for the E and B asymmetry and the CℓTE/CℓEE ratio, reported in the power spectra analysis of the Planck353 GHz polarization maps. Future models of the dust foreground for CMB polarization studies will need to take into account the observed correlation between the dust polarization and the structure of interstellar matter.
AB - The quest for a B-mode imprint from primordial gravity waves on the polarization of the cosmic microwave background (CMB) requires the characterization of foreground polarization from Galactic dust. We present a statistical study of the filamentary structure of the 353 GHz Planck Stokes maps at high Galactic latitude, relevant to the study of dust emission as a polarized foreground to the CMB. We filter the intensity and polarization maps to isolate filaments in the range of angular scales where the power asymmetry between E-modes and B-modes is observed. Using the Smoothed Hessian Major Axis Filament Finder (SMAFF), we identify 259 filaments at high Galactic latitude, with lengths larger or equal to 2° (corresponding to 3.5 pc in length for a typical distance of 100 pc). These filaments show a preferred orientation parallel to the magnetic field projected onto the plane of the sky, derived from their polarization angles. We present mean maps of the filaments in Stokes I, Q, U, E, and B, computed by stacking individual images rotated to align the orientations of the filaments. Combining the stacked images and the histogram of relative orientations, we estimate the mean polarization fraction of the filaments to be 11%. Furthermore, we show that the correlation between the filaments and the magnetic field orientations may account for the E and B asymmetry and the CℓTE/CℓEE ratio, reported in the power spectra analysis of the Planck353 GHz polarization maps. Future models of the dust foreground for CMB polarization studies will need to take into account the observed correlation between the dust polarization and the structure of interstellar matter.
KW - Galaxies: ISM
KW - ISM: general
KW - Polarization
KW - Submillimeter: ISM
UR - http://www.scopus.com/inward/record.url?scp=84958948576&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84958948576&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201526506
DO - 10.1051/0004-6361/201526506
M3 - Article
AN - SCOPUS:84958948576
VL - 586
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A141
ER -