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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 11604naa a2202401 4500 | |
| 001 | oai:DiVA.org:su-186398 | |
| 003 | SwePub | |
| 008 | 201109s2020 | |||||||||||000 ||eng| | |
| 009 | oai:DiVA.org:kth-287189 | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1863982 URI |
| 024 | 7 | a https://doi.org/10.1051/0004-6361/2018338852 DOI |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-2871892 URI |
| 040 | a (SwePub)sud (SwePub)kth | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a art2 swepub-publicationtype |
| 100 | 1 | a Aghanim, N.4 aut |
| 245 | 1 0 | a Planck 2018 results XII. Galactic astrophysics using polarized dust emission |
| 264 | c 2020-09-11 | |
| 264 | 1 | b EDP Sciences,c 2020 |
| 338 | a print2 rdacarrier | |
| 500 | a Nordita SU, QC 20211006 | |
| 520 | a Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle psi, and dispersion function of polarization angles ?. The joint distribution (one-point statistics) of p and N-H confirms that the mean and maximum polarization fractions decrease with increasing N-H. The uncertainty on the maximum observed polarization fraction, (max) = 22.0(-1.4)(+3.5) p max = 22 . 0 - 1.4 + 3.5 % at 353 GHz and 80 ' resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and ? found earlier is seen to be present at high latitudes. This follows the ?proportional to p(-1) relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, psi, and ? for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map ?xp, looking for residual trends. While the polarization fraction p decreases by a factor of 3-4 between N-H=10(20) cm(-2) and N-H=2x10(22) cm(-2), out of the Galactic plane, this product ?xp only decreases by about 25%. Because ? is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with N-H is determined mostly by the magnetic-field structure and not by a drop in grain alignment. This systematic trend is observed both in the diffuse interstellar medium (ISM) and in molecular clouds of the Gould Belt. Second, we look for a dependence of polarization properties on the dust temperature, as we would expect from the radiative alignment torque (RAT) theory. We find no systematic trend of ?xp with the dust temperature T-d, whether in the diffuse ISM or in the molecular clouds of the Gould Belt. In the diffuse ISM, lines of sight with high polarization fraction p and low polarization angle dispersion ? tend, on the contrary, to have colder dust than lines of sight with low p and high ?. We also compare the Planck thermal dust polarization with starlight polarization data in the visible at high Galactic latitudes. The agreement in polarization angles is remarkable, and is consistent with what we expect from the noise and the observed dispersion of polarization angles in the visible on the scale of the Planck beam. The two polarization emission-to-extinction ratios, R-P/p and R-S/V, which primarily characterize dust optical properties, have only a weak dependence on the column density, and converge towards the values previously determined for translucent lines of sight. We also determine an upper limit for the polarization fraction in extinction, p(V)/E(B-V), of 13% at high Galactic latitude, compatible with the polarization fraction p approximate to 20% observed at 353 GHz. Taken together, these results provide strong constraints for models of Galactic dust in diffuse gas. | |
| 650 | 7 | a NATURVETENSKAPx Fysik0 (SwePub)1032 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciences0 (SwePub)1032 hsv//eng |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 653 | a polarization | |
| 653 | a magnetic fields | |
| 653 | a turbulence | |
| 653 | a dust | |
| 653 | a extinction | |
| 653 | a local insterstellar matter | |
| 653 | a submillimeter: ISM | |
| 700 | 1 | a Akrami, Y.4 aut |
| 700 | 1 | a Alves, M. I. R.4 aut |
| 700 | 1 | a Ashdown, M.4 aut |
| 700 | 1 | a Aumont, J.4 aut |
| 700 | 1 | a Baccigalupi, C.4 aut |
| 700 | 1 | a Ballardini, M.4 aut |
| 700 | 1 | a Banday, A. J.4 aut |
| 700 | 1 | a Barreiro, R. B.4 aut |
| 700 | 1 | a Bartolo, N.4 aut |
| 700 | 1 | a Basak, S.4 aut |
| 700 | 1 | a Benabed, K.4 aut |
| 700 | 1 | a Bernard, J. -P.4 aut |
| 700 | 1 | a Bersanelli, M.4 aut |
| 700 | 1 | a Bielewicz, P.4 aut |
| 700 | 1 | a Bock, J. J.4 aut |
| 700 | 1 | a Bond, J. R.4 aut |
| 700 | 1 | a Borrill, J.4 aut |
| 700 | 1 | a Bouchet, F. R.4 aut |
| 700 | 1 | a Boulanger, F.4 aut |
| 700 | 1 | a Bracco, Andreau Stockholms universitet,Nordiska institutet för teoretisk fysik (Nordita),Université Paris-Saclay, France,Nordita SU4 aut0 (Swepub:su)abrac |
| 700 | 1 | a Bucher, M.4 aut |
| 700 | 1 | a Burigana, C.4 aut |
| 700 | 1 | a Calabrese, E.4 aut |
| 700 | 1 | a Cardoso, J. -F.4 aut |
| 700 | 1 | a Carron, J.4 aut |
| 700 | 1 | a Chary, R. -R.4 aut |
| 700 | 1 | a Chiang, H. C.4 aut |
| 700 | 1 | a Colombo, L. P. L.4 aut |
| 700 | 1 | a Combet, C.4 aut |
| 700 | 1 | a Crill, B. P.4 aut |
| 700 | 1 | a Cuttaia, F.4 aut |
| 700 | 1 | a de Bernardis, P.4 aut |
| 700 | 1 | a de Zotti, G.4 aut |
| 700 | 1 | a Delabrouille, J.4 aut |
| 700 | 1 | a Delouis, J. -M.4 aut |
| 700 | 1 | a Di Valentino, E.4 aut |
| 700 | 1 | a Dickinson, C.4 aut |
| 700 | 1 | a Diego, J. M.4 aut |
| 700 | 1 | a Dore, O.4 aut |
| 700 | 1 | a Douspis, M.4 aut |
| 700 | 1 | a Ducout, A.4 aut |
| 700 | 1 | a Dupac, X.4 aut |
| 700 | 1 | a Gudmundsson, Jón E.u Stockholms universitet,Fysikum,Oskar Klein-centrum för kosmopartikelfysik (OKC),Princeton University, USA4 aut0 (Swepub:su)jgudm |
| 700 | 1 | a Elsner, F.4 aut |
| 700 | 1 | a Ensslin, T. A.4 aut |
| 700 | 1 | a Eriksen, H. K.4 aut |
| 700 | 1 | a Falgarone, E.4 aut |
| 700 | 1 | a Fantaye, Y.4 aut |
| 700 | 1 | a Fernandez-Cobos, R.4 aut |
| 700 | 1 | a Ferriere, K.4 aut |
| 700 | 1 | a Finelli, F.4 aut |
| 700 | 1 | a Forastieri, F.4 aut |
| 700 | 1 | a Frailis, M.4 aut |
| 700 | 1 | a Fraisse, A. A.4 aut |
| 700 | 1 | a Franceschi, E.4 aut |
| 700 | 1 | a Frolov, A.4 aut |
| 700 | 1 | a Galeotta, S.4 aut |
| 700 | 1 | a Galli, S.4 aut |
| 700 | 1 | a Ganga, K.4 aut |
| 700 | 1 | a Genova-Santos, R. T.4 aut |
| 700 | 1 | a Gerbino, Martinau Stockholms universitet,Fysikum,Oskar Klein-centrum för kosmopartikelfysik (OKC)4 aut0 (Swepub:su)mgerb |
| 700 | 1 | a Ghosh, T.4 aut |
| 700 | 1 | a Gonzalez-Nuevo, J.4 aut |
| 700 | 1 | a Gorski, K. M.4 aut |
| 700 | 1 | a Gratton, S.4 aut |
| 700 | 1 | a Green, G.4 aut |
| 700 | 1 | a Gruppuso, A.4 aut |
| 700 | 1 | a Gudmundsson, Jón E.u Stockholms universitet,Fysikum,Oskar Klein-centrum för kosmopartikelfysik (OKC),Princeton University, USA4 aut0 (Swepub:su)jgudm |
| 700 | 1 | a Guillet, V.4 aut |
| 700 | 1 | a Handley, W.4 aut |
| 700 | 1 | a Hansen, F. K.4 aut |
| 700 | 1 | a Helou, G.4 aut |
| 700 | 1 | a Herranz, D.4 aut |
| 700 | 1 | a Hivon, E.4 aut |
| 700 | 1 | a Huang, Z.4 aut |
| 700 | 1 | a Jaffe, A. H.4 aut |
| 700 | 1 | a Jones, W. C.4 aut |
| 700 | 1 | a Keihanen, E.4 aut |
| 700 | 1 | a Keskitalo, R.4 aut |
| 700 | 1 | a Kiiveri, K.4 aut |
| 700 | 1 | a Kim, J.4 aut |
| 700 | 1 | a Krachmalnicoff, N.4 aut |
| 700 | 1 | a Kunz, M.4 aut |
| 700 | 1 | a Kurki-Suonio, H.4 aut |
| 700 | 1 | a Lagache, G.4 aut |
| 700 | 1 | a Lamarre, J. -M.4 aut |
| 700 | 1 | a Lasenby, A.4 aut |
| 700 | 1 | a Lattanzi, M.4 aut |
| 700 | 1 | a Lawrence, C. R.4 aut |
| 700 | 1 | a Le Jeune, M.4 aut |
| 700 | 1 | a Levrier, F.4 aut |
| 700 | 1 | a Liguori, M.4 aut |
| 700 | 1 | a Lilje, P. B.4 aut |
| 700 | 1 | a Lindholm, V.4 aut |
| 700 | 1 | a Lopez-Caniego, M.4 aut |
| 700 | 1 | a Lubin, P. M.4 aut |
| 700 | 1 | a Ma, Y. -Z.4 aut |
| 700 | 1 | a Macias-Perez, J. F.4 aut |
| 700 | 1 | a Maggio, G.4 aut |
| 700 | 1 | a Maino, D.4 aut |
| 700 | 1 | a Mandolesi, N.4 aut |
| 700 | 1 | a Mangilli, A.4 aut |
| 700 | 1 | a Marcos-Caballero, A.4 aut |
| 700 | 1 | a Maris, M.4 aut |
| 700 | 1 | a Martin, P. G.4 aut |
| 700 | 1 | a Martinez-Gonzalez, E.4 aut |
| 700 | 1 | a Matarrese, S.4 aut |
| 700 | 1 | a Mauri, N.4 aut |
| 700 | 1 | a McEwen, J. D.4 aut |
| 700 | 1 | a Melchiorri, A.4 aut |
| 700 | 1 | a Mennella, A.4 aut |
| 700 | 1 | a Migliaccio, M.4 aut |
| 700 | 1 | a Miville-Deschenes, M. -A.4 aut |
| 700 | 1 | a Molinari, D.4 aut |
| 700 | 1 | a Moneti, A.4 aut |
| 700 | 1 | a Montier, L.4 aut |
| 700 | 1 | a Morgante, G.4 aut |
| 700 | 1 | a Moss, A.4 aut |
| 700 | 1 | a Natoli, P.4 aut |
| 700 | 1 | a Pagano, L.4 aut |
| 700 | 1 | a Paoletti, D.4 aut |
| 700 | 1 | a Patanchon, G.4 aut |
| 700 | 1 | a Perrotta, F.4 aut |
| 700 | 1 | a Pettorino, V.4 aut |
| 700 | 1 | a Piacentini, F.4 aut |
| 700 | 1 | a Polastri, L.4 aut |
| 700 | 1 | a Polenta, G.4 aut |
| 700 | 1 | a Puget, J. -L.4 aut |
| 700 | 1 | a Rachen, J. P.4 aut |
| 700 | 1 | a Reinecke, M.4 aut |
| 700 | 1 | a Remazeilles, M.4 aut |
| 700 | 1 | a Renzi, A.4 aut |
| 700 | 1 | a Ristorcelli, I.4 aut |
| 700 | 1 | a Rocha, G.4 aut |
| 700 | 1 | a Rosset, C.4 aut |
| 700 | 1 | a Roudier, G.4 aut |
| 700 | 1 | a Rubino-Martin, J. A.4 aut |
| 700 | 1 | a Ruiz-Granados, B.4 aut |
| 700 | 1 | a Salvati, L.4 aut |
| 700 | 1 | a Sandri, M.4 aut |
| 700 | 1 | a Savelainen, M.4 aut |
| 700 | 1 | a Scott, D.4 aut |
| 700 | 1 | a Sirignano, C.4 aut |
| 700 | 1 | a Sunyaev, R.4 aut |
| 700 | 1 | a Suur-Uski, A. -S.4 aut |
| 700 | 1 | a Tauber, J. A.4 aut |
| 700 | 1 | a Tavagnacco, D.4 aut |
| 700 | 1 | a Tenti, M.4 aut |
| 700 | 1 | a Toffolatti, L.4 aut |
| 700 | 1 | a Tomasi, M.4 aut |
| 700 | 1 | a Trombetti, T.4 aut |
| 700 | 1 | a Valiviita, J.4 aut |
| 700 | 1 | a Vansyngel, F.4 aut |
| 700 | 1 | a Van Tent, B.4 aut |
| 700 | 1 | a Vielva, P.4 aut |
| 700 | 1 | a Villa, F.4 aut |
| 700 | 1 | a Vittorio, N.4 aut |
| 700 | 1 | a Wandelt, B. D.4 aut |
| 700 | 1 | a Wehus, I. K.4 aut |
| 700 | 1 | a Zacchei, A.4 aut |
| 700 | 1 | a Zonca, A.4 aut |
| 710 | 2 | a Stockholms universitetb Nordiska institutet för teoretisk fysik (Nordita)4 org |
| 773 | 0 | t Astronomy and Astrophysicsd : EDP Sciencesg 641q 641x 0004-6361x 1432-0746 |
| 856 | 4 | u https://doi.org/10.1051/0004-6361/201833885y Fulltext |
| 856 | 4 | u https://www.aanda.org/articles/aa/pdf/2020/09/aa33885-18.pdf |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-186398 |
| 856 | 4 8 | u https://doi.org/10.1051/0004-6361/201833885 |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-287189 |
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- Aghanim, N.
- Akrami, Y.
- Alves, M. I. R.
- Ashdown, M.
- Aumont, J.
- Baccigalupi, C.
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- Ballardini, M.
- Banday, A. J.
- Barreiro, R. B.
- Bartolo, N.
- Basak, S.
- Benabed, K.
- Bernard, J. -P.
- Bersanelli, M.
- Bielewicz, P.
- Bock, J. J.
- Bond, J. R.
- Borrill, J.
- Bouchet, F. R.
- Boulanger, F.
- Bracco, Andrea
- Bucher, M.
- Burigana, C.
- Calabrese, E.
- Cardoso, J. -F.
- Carron, J.
- Chary, R. -R.
- Chiang, H. C.
- Colombo, L. P. L ...
- Combet, C.
- Crill, B. P.
- Cuttaia, F.
- de Bernardis, P.
- de Zotti, G.
- Delabrouille, J.
- Delouis, J. -M.
- Di Valentino, E.
- Dickinson, C.
- Diego, J. M.
- Dore, O.
- Douspis, M.
- Ducout, A.
- Dupac, X.
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- Elsner, F.
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- Eriksen, H. K.
- Falgarone, E.
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- Fernandez-Cobos, ...
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- Finelli, F.
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- Gruppuso, A.
- Guillet, V.
- Handley, W.
- Hansen, F. K.
- Helou, G.
- Herranz, D.
- Hivon, E.
- Huang, Z.
- Jaffe, A. H.
- Jones, W. C.
- Keihanen, E.
- Keskitalo, R.
- Kiiveri, K.
- Kim, J.
- Krachmalnicoff, ...
- Kunz, M.
- Kurki-Suonio, H.
- Lagache, G.
- Lamarre, J. -M.
- Lasenby, A.
- Lattanzi, M.
- Lawrence, C. R.
- Le Jeune, M.
- Levrier, F.
- Liguori, M.
- Lilje, P. B.
- Lindholm, V.
- Lopez-Caniego, M ...
- Lubin, P. M.
- Ma, Y. -Z.
- Macias-Perez, J. ...
- Maggio, G.
- Maino, D.
- Mandolesi, N.
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- Martinez-Gonzale ...
- Matarrese, S.
- Mauri, N.
- McEwen, J. D.
- Melchiorri, A.
- Mennella, A.
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- Molinari, D.
- Moneti, A.
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- Morgante, G.
- Moss, A.
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- Patanchon, G.
- Perrotta, F.
- Pettorino, V.
- Piacentini, F.
- Polastri, L.
- Polenta, G.
- Puget, J. -L.
- Rachen, J. P.
- Reinecke, M.
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- Tauber, J. A.
- Tavagnacco, D.
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- Vansyngel, F.
- Van Tent, B.
- Vielva, P.
- Villa, F.
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- Wehus, I. K.
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