Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

P. A.R. Ade; N. Aghanim; D. Alina; M. I.R. Alves; G. Aniano; C. Armitage-Caplan; M. Arnaud; D. Arzoumanian; M. Ashdown; F. Atrio-Barandela; J. Aumont; C. Baccigalupi; A. J. Banday; R. B. Barreiro; E. Battaner; K. Benabed; A. Benoit-Lévy; J. P. Bernard; M. Bersanelli; P. Bielewicz; J. R. Bond; J. Borrill; F. R. Bouchet; F. Boulanger; A. Bracco; C. Burigana; J. F. Cardoso; A. Catalano; A. Chamballu; H. C. Chiang; P. R. Christensen; 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; A. De Rosa; G. De Zotti; J. Delabrouille; C. Dickinson; J. M. Diego; S. Donzelli; O. Doré; M. Douspis; X. Dupac; G. Efstathiou; T. A. Enßlin; H. K. Eriksen; E. Falgarone; L. Fanciullo; K. Ferrière; F. Finelli; O. Forni; M. Frailis; A. A. Fraisse; E. Franceschi; S. Galeotta; K. Ganga; T. Ghosh; M. Giard; Y. Giraud-Héraud; J. González-Nuevo; K. M. Górski; A. Gregorio; A. Gruppuso; V. Guillet; F. K. Hansen; D. L. Harrison; G. Helou; C. Hernández-Monteagudo; S. R. Hildebrandt; E. Hivon; M. Hobson; W. A. Holmes; A. Hornstrup; K. M. Huffenberger; A. H. Jaffe; T. R. Jaffe; W. C. Jones; M. Juvela; E. Keihänen; R. Keskitalo; T. S. Kisner; R. Kneissl; J. Knoche; M. Kunz; H. Kurki-Suonio; G. Lagache; J. M. Lamarre; A. Lasenby; C. R. Lawrence; R. Leonardi; F. Levrier; M. Liguori; P. B. Lilje; M. Linden-Vørnle; M. López-Caniego; P. M. Lubin; J. F. Macías-Pérez; D. Maino; N. Mandolesi; M. Maris; D. J. Marshall; P. G. Martin; E. Martínez-González; S. Masi; S. Matarrese; P. Mazzotta; A. Melchiorri; L. Mendes; A. Mennella; M. Migliaccio; M. A. Miville-Deschênes; A. Moneti; L. Montier; G. Morgante; D. Mortlock; D. Munshi; J. A. Murphy; P. Naselsky; F. Nati; P. Natoli; C. B. Netterfield; F. Noviello; D. Novikov; I. Novikov; C. A. Oxborrow; L. Pagano; F. Pajot; D. Paoletti; F. Pasian; V. M. Pelkonen; O. Perdereau; L. Perotto; F. Perrotta; F. Piacentini; M. Piat; D. Pietrobon; S. Plaszczynski; E. Pointecouteau; G. Polenta; L. Popa; G. W. Pratt; S. Prunet; J. L. Puget; J. P. Rachen; M. Reinecke; M. Remazeilles; C. Renault; S. Ricciardi; T. Riller; I. Ristorcelli; G. Rocha; C. Rosset; G. Roudier; B. Rusholme; M. Sandri; D. Scott; J. D. Soler; L. D. Spencer; V. Stolyarov; R. Stompor; R. Sudiwala; D. Sutton; A. S. Suur-Uski; J. F. Sygnet; J. A. Tauber; L. Terenzi; L. Toffolatti; M. Tomasi; M. Tristram; M. Tucci; G. Umana; L. Valenziano; J. Valiviita; B. Van Tent; P. Vielva; F. Villa; L. A. Wade; B. D. Wandelt; A. Zonca

doi:10.1051/0004-6361/201424086

Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

P. A.R. Ade, N. Aghanim, D. Alina, M. I.R. Alves, G. Aniano, C. Armitage-Caplan, M. Arnaud, D. Arzoumanian, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, K. Benabed, A. Benoit-Lévy, J. P. Bernard, M. Bersanelli, P. BielewiczJ. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, A. Bracco, C. Burigana, J. F. Cardoso, A. Catalano, A. Chamballu, H. C. Chiang, P. R. Christensen, 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, A. De Rosa, G. De Zotti, J. Delabrouille, C. Dickinson, J. M. Diego, S. Donzelli, O. Doré, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, E. Falgarone, L. Fanciullo, K. Ferrière, F. Finelli, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, S. Galeotta, K. Ganga, T. Ghosh, M. Giard, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, A. Gregorio, A. Gruppuso, V. Guillet, F. K. Hansen, D. L. Harrison, G. Helou, C. Hernández-Monteagudo, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, A. Hornstrup, K. M. Huffenberger, A. H. Jaffe, T. R. Jaffe, W. C. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, M. Kunz, H. Kurki-Suonio, G. Lagache, J. M. Lamarre, A. Lasenby, C. R. Lawrence, R. Leonardi, F. Levrier, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. Macías-Pérez, D. Maino, N. Mandolesi, M. Maris, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, S. Matarrese, P. Mazzotta, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, M. A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, F. Noviello, D. Novikov, I. Novikov, C. A. Oxborrow, L. Pagano, F. Pajot, D. Paoletti, F. Pasian, V. M. Pelkonen, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, L. Popa, G. W. Pratt, S. Prunet, J. L. Puget, J. P. Rachen, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, B. Rusholme, M. Sandri, D. Scott, J. D. Soler, L. D. Spencer, V. Stolyarov, R. Stompor, R. Sudiwala, D. Sutton, A. S. Suur-Uski, J. F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Tucci, G. Umana, L. Valenziano, J. Valiviita, B. Van Tent, P. Vielva, F. Villa, L. A. Wade, B. D. Wandelt, A. Zonca

Physics

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

35 Scopus citations

Abstract

Polarized emission observed by Planck HFI at 353? GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles ψ. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction p_max decreases with column density N_H in the more opaque fields with N_H> 10²¹ cm^-2; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction p_max in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function S. However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties.

Original language	English (US)
Article number	A105
Journal	Astronomy and Astrophysics
Volume	576
DOIs	https://doi.org/10.1051/0004-6361/201424086
State	Published - Apr 1 2015

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Dust, extinction
ISM: clouds
ISM: general
ISM: magnetic fields
Infrared: ISM
Submillimeter: ISM

Access to Document

10.1051/0004-6361/201424086

Cite this

Ade, P. A. R., Aghanim, N., Alina, D., Alves, M. I. R., Aniano, G., Armitage-Caplan, C., Arnaud, M., Arzoumanian, D., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J. P., Bersanelli, M., ... Zonca, A. (2015). Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence. Astronomy and Astrophysics, 576, Article A105. https://doi.org/10.1051/0004-6361/201424086

@article{560bd34963f14c5ea0d804d3bc34702a,

title = "Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence",

abstract = "Polarized emission observed by Planck HFI at 353? GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles ψ. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction pmax decreases with column density NH in the more opaque fields with NH> 1021 cm-2; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction pmax in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function S. However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties.",

keywords = "Dust, extinction, ISM: clouds, ISM: general, ISM: magnetic fields, Infrared: ISM, Submillimeter: ISM",

author = "Ade, {P. A.R.} and N. Aghanim and D. Alina and Alves, {M. I.R.} and G. Aniano and C. Armitage-Caplan and M. Arnaud and D. Arzoumanian and M. Ashdown and F. Atrio-Barandela and J. Aumont and C. Baccigalupi and Banday, {A. J.} and Barreiro, {R. B.} and E. Battaner and K. Benabed and A. Benoit-L{\'e}vy and Bernard, {J. P.} and M. Bersanelli and P. Bielewicz and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} and F. Boulanger and A. Bracco and C. Burigana and Cardoso, {J. F.} and A. Catalano and A. Chamballu and Chiang, {H. C.} and Christensen, {P. R.} 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 Rosa}, A. and {De Zotti}, G. and J. Delabrouille and C. Dickinson and Diego, {J. M.} and S. Donzelli and O. Dor{\'e} and M. Douspis and X. Dupac and G. Efstathiou and En{\ss}lin, {T. A.} and Eriksen, {H. K.} and E. Falgarone and L. Fanciullo and K. Ferri{\`e}re and F. Finelli and O. Forni and M. Frailis and Fraisse, {A. A.} and E. Franceschi and S. Galeotta and K. Ganga and T. Ghosh and M. Giard and Y. Giraud-H{\'e}raud and J. Gonz{\'a}lez-Nuevo and G{\'o}rski, {K. M.} and A. Gregorio and A. Gruppuso and V. Guillet and Hansen, {F. K.} and Harrison, {D. L.} and G. Helou and C. Hern{\'a}ndez-Monteagudo and Hildebrandt, {S. R.} and E. Hivon and M. Hobson and Holmes, {W. A.} and A. Hornstrup and Huffenberger, {K. M.} and Jaffe, {A. H.} and Jaffe, {T. R.} and Jones, {W. C.} and M. Juvela and E. Keih{\"a}nen and R. Keskitalo and Kisner, {T. S.} and R. Kneissl and J. Knoche and M. Kunz and H. Kurki-Suonio and G. Lagache and Lamarre, {J. M.} and A. Lasenby and Lawrence, {C. R.} and R. Leonardi and F. Levrier and M. Liguori and Lilje, {P. B.} and M. Linden-V{\o}rnle and M. L{\'o}pez-Caniego and Lubin, {P. M.} and Mac{\'i}as-P{\'e}rez, {J. F.} and D. Maino and N. Mandolesi and M. Maris and Marshall, {D. J.} and Martin, {P. G.} and E. Mart{\'i}nez-Gonz{\'a}lez and S. Masi and S. Matarrese and P. Mazzotta and A. Melchiorri and L. Mendes and A. Mennella and M. Migliaccio and Miville-Desch{\^e}nes, {M. A.} and A. Moneti and L. Montier and G. Morgante and D. Mortlock and D. Munshi and Murphy, {J. A.} and P. Naselsky and F. Nati and P. Natoli and Netterfield, {C. B.} and F. Noviello and D. Novikov and I. Novikov and Oxborrow, {C. A.} and L. Pagano and F. Pajot and D. Paoletti and F. Pasian and Pelkonen, {V. M.} and O. Perdereau and L. Perotto and F. Perrotta and F. Piacentini and M. Piat and D. Pietrobon and S. Plaszczynski and E. Pointecouteau and G. Polenta and L. Popa and Pratt, {G. W.} and S. Prunet and Puget, {J. L.} and Rachen, {J. P.} and M. Reinecke and M. Remazeilles and C. Renault and S. Ricciardi and T. Riller and I. Ristorcelli and G. Rocha and C. Rosset and G. Roudier and B. Rusholme and M. Sandri and D. Scott and Soler, {J. D.} and Spencer, {L. D.} and V. Stolyarov and R. Stompor and R. Sudiwala and D. Sutton and Suur-Uski, {A. S.} and Sygnet, {J. F.} and Tauber, {J. A.} and L. Terenzi and L. Toffolatti and M. Tomasi and M. Tristram and M. Tucci and G. Umana and L. Valenziano and J. Valiviita and {Van Tent}, B. and P. Vielva and F. Villa and Wade, {L. A.} and Wandelt, {B. D.} and A. Zonca",

note = "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, 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); 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.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration . Some of the results in this paper have been derived using the HEALPix package. The authors would like to thank Charles Beichman for his careful reading of the manuscript and useful comments. The research leading to these results has received funding from the European Research Council under the European Union{\textquoteright}s Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement No. 267934. Publisher Copyright: {\textcopyright} ESO, 2015.",

year = "2015",

month = apr,

day = "1",

doi = "10.1051/0004-6361/201424086",

language = "English (US)",

volume = "576",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Ade, PAR, Aghanim, N, Alina, D, Alves, MIR, Aniano, G, Armitage-Caplan, C, Arnaud, M, Arzoumanian, D, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Battaner, E, Benabed, K, Benoit-Lévy, A, Bernard, JP, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Burigana, C, Cardoso, JF, Catalano, A, Chamballu, A, Chiang, HC, Christensen, PR, 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 Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, JM, Donzelli, S, Doré, O, Douspis, M, Dupac, X, Efstathiou, G, Enßlin, TA, Eriksen, HK, Falgarone, E, Fanciullo, L, Ferrière, K, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, FK, Harrison, DL, Helou, G, Hernández-Monteagudo, C, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Huffenberger, KM, Jaffe, AH, Jaffe, TR, Jones, WC, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Lawrence, CR, Leonardi, R, Levrier, F, Liguori, M, Lilje, PB, Linden-Vørnle, M, López-Caniego, M, Lubin, PM, Macías-Pérez, JF, Maino, D, Mandolesi, N, Maris, M, Marshall, DJ, Martin, PG, Martínez-González, E, Masi, S, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Miville-Deschênes, MA, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, JA, Naselsky, P, Nati, F, Natoli, P, Netterfield, CB, Noviello, F, Novikov, D, Novikov, I, Oxborrow, CA, Pagano, L, Pajot, F, Paoletti, D, Pasian, F, Pelkonen, VM, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Popa, L, Pratt, GW, Prunet, S, Puget, JL, Rachen, JP, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rusholme, B, Sandri, M, Scott, D, Soler, JD, Spencer, LD, Stolyarov, V, Stompor, R, Sudiwala, R, Sutton, D, Suur-Uski, AS, Sygnet, JF, Tauber, JA, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wade, LA, Wandelt, BD & Zonca, A 2015, 'Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence', Astronomy and Astrophysics, vol. 576, A105. https://doi.org/10.1051/0004-6361/201424086

TY - JOUR

T1 - Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

AU - Ade, P. A.R.

AU - Aghanim, N.

AU - Alina, D.

AU - Alves, M. I.R.

AU - Aniano, G.

AU - Armitage-Caplan, C.

AU - Arnaud, M.

AU - Arzoumanian, D.

AU - Ashdown, M.

AU - Atrio-Barandela, F.

AU - Aumont, J.

AU - Baccigalupi, C.

AU - Banday, A. J.

AU - Barreiro, R. B.

AU - Battaner, E.

AU - Benabed, K.

AU - Benoit-Lévy, A.

AU - Bernard, J. P.

AU - Bersanelli, M.

AU - Bielewicz, P.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Boulanger, F.

AU - Bracco, A.

AU - Burigana, C.

AU - Cardoso, J. F.

AU - Catalano, A.

AU - Chamballu, A.

AU - Chiang, H. C.

AU - Christensen, P. R.

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 Rosa, A.

AU - De Zotti, G.

AU - Delabrouille, J.

AU - Dickinson, C.

AU - Diego, J. M.

AU - Donzelli, S.

AU - Doré, O.

AU - Douspis, M.

AU - Dupac, X.

AU - Efstathiou, G.

AU - Enßlin, T. A.

AU - Eriksen, H. K.

AU - Falgarone, E.

AU - Fanciullo, L.

AU - Ferrière, K.

AU - Finelli, F.

AU - Forni, O.

AU - Frailis, M.

AU - Fraisse, A. A.

AU - Franceschi, E.

AU - Galeotta, S.

AU - Ganga, K.

AU - Ghosh, T.

AU - Giard, M.

AU - Giraud-Héraud, Y.

AU - González-Nuevo, J.

AU - Górski, K. M.

AU - Gregorio, A.

AU - Gruppuso, A.

AU - Guillet, V.

AU - Hansen, F. K.

AU - Harrison, D. L.

AU - Helou, G.

AU - Hernández-Monteagudo, C.

AU - Hildebrandt, S. R.

AU - Hivon, E.

AU - Hobson, M.

AU - Holmes, W. A.

AU - Hornstrup, A.

AU - Huffenberger, K. M.

AU - Jaffe, A. H.

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 - Lagache, G.

AU - Lamarre, J. M.

AU - Lasenby, A.

AU - Lawrence, C. R.

AU - Leonardi, R.

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 - Maino, D.

AU - Mandolesi, N.

AU - Maris, M.

AU - Marshall, D. J.

AU - Martin, P. G.

AU - Martínez-González, E.

AU - Masi, S.

AU - Matarrese, S.

AU - Mazzotta, P.

AU - Melchiorri, A.

AU - Mendes, L.

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 - Netterfield, C. B.

AU - Noviello, F.

AU - Novikov, D.

AU - Novikov, I.

AU - Oxborrow, C. A.

AU - Pagano, L.

AU - Pajot, F.

AU - Paoletti, D.

AU - Pasian, F.

AU - Pelkonen, V. M.

AU - Perdereau, O.

AU - Perotto, L.

AU - Perrotta, F.

AU - Piacentini, F.

AU - Piat, M.

AU - Pietrobon, D.

AU - Plaszczynski, S.

AU - Pointecouteau, E.

AU - Polenta, G.

AU - Popa, L.

AU - Pratt, G. W.

AU - Prunet, S.

AU - Puget, J. L.

AU - Rachen, J. P.

AU - Reinecke, M.

AU - Remazeilles, M.

AU - Renault, C.

AU - Ricciardi, S.

AU - Riller, T.

AU - Ristorcelli, I.

AU - Rocha, G.

AU - Rosset, C.

AU - Roudier, G.

AU - Rusholme, B.

AU - Sandri, M.

AU - Scott, D.

AU - Soler, J. D.

AU - Spencer, L. D.

AU - Stolyarov, V.

AU - Stompor, R.

AU - Sudiwala, 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 - 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 - 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, 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); 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.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration . Some of the results in this paper have been derived using the HEALPix package. The authors would like to thank Charles Beichman for his careful reading of the manuscript and useful comments. 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, 2015.

PY - 2015/4/1

Y1 - 2015/4/1

N2 - Polarized emission observed by Planck HFI at 353? GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles ψ. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction pmax decreases with column density NH in the more opaque fields with NH> 1021 cm-2; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction pmax in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function S. However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties.

AB - Polarized emission observed by Planck HFI at 353? GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles ψ. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction pmax decreases with column density NH in the more opaque fields with NH> 1021 cm-2; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction pmax in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function S. However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties.

KW - Dust, extinction

KW - ISM: clouds

KW - ISM: general

KW - ISM: magnetic fields

KW - Infrared: ISM

KW - Submillimeter: ISM

UR - http://www.scopus.com/inward/record.url?scp=84928032459&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84928032459&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201424086

DO - 10.1051/0004-6361/201424086

M3 - Article

AN - SCOPUS:84928032459

SN - 0004-6361

VL - 576

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A105

ER -

Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

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