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Planck intermediate results. XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust

Planck Collaboration R. Adam 1 R. Ade N. Aghanim 2 R. Alves M. Arnaud D. Arzoumanian 2 M. Ashdown J. Aumont C. Baccigalupi J. Banday R. Barreiro N. Bartolo E. Battaner K. Benabed A. Benoit-Lévy 3 M. Bersanelli P. Bielewicz 4 A. Bonaldi L. Bonavera R. Bond J. Borrill R. Bouchet 3 F. Boulanger A. Bracco C. Burigana R. Butler E. Calabrese J. Cardoso 5 A. Catalano 1, 6 A. Chamballu C. Chiang R. Christensen S. Colombi P. Colombo C. Combet 1 F. Couchot 7 P. Crill A. Curto F. Cuttaia L. Danese R. Davies R. Davis P. Bernard A. de Rosa G. de Zotti J. Delabrouille 5 C. Dickinson M. Diego H. Dole 2 S. Donzelli O. Doré M. Douspis 2 A. Ducout 3 X. Dupac G. Efstathiou F. Elsner A. Enßlin K. Eriksen E. Falgarone 6 K. Ferrière F. Finelli O. Forni 4 M. Frailis A. Fraisse E. Franceschi A. Frejsel S. Galeotta S. Galli K. Ganga 5 T. Ghosh M. Giard 4 E. Gjerløw J. González-Nuevo M. Górski A. Gregorio A. Gruppuso V. Guillet 2 K. Hansen D. Hanson D. Harrison S. Henrot-Versillé 7 C. Hernández-Monteagudo D. Herranz R. Hildebrandt E. Hivon 3 M. Hobson A. Holmes W. Hovest M. Huffenberger G. Hurier A. Jaffe R. Jaffe C. Jones M. Juvela E. Keihänen R. Keskitalo S. Kisner R. Kneissl J. Knoche M. Kunz 2 H. Kurki-Suonio Guilaine Lagache 8 M. Lamarre 6 A. Lasenby M. Lattanzi R. Lawrence R. Leonardi F. Levrier 6 M. Liguori P. Lilje M. Linden-Vørnle M. López-Caniego P. Lubin J. Macias-Perez 1 B. Maffei D. Maino N. Mandolesi M. Maris D. Marshall P. Martin E. Martínez-González S. Masi S. Matarrese P. Mazzotta A. Melchiorri L. Mendes A. Mennella M. Migliaccio M. Miville-Deschênes A. Moneti L. Montier 4 G. Morgante D. Mortlock D. Munshi J. Murphy P. Naselsky P. Natoli H. Nørgaard-Nielsen F. Noviello 2 D. Novikov I. Novikov N. Oppermann C. Oxborrow L. Pagano F. Pajot 2 D. Paoletti F. Pasian O. Perdereau 7 L. Perotto 1 F. Perrotta V. Pettorino 9 F. Piacentini M. Piat 5 S. Plaszczynski 7 E. Pointecouteau 4 G. Polenta N. Ponthieu L. Popa G. Pratt 10 S. Prunet J. Puget P. Rachen T. Reach M. Reinecke M. Remazeilles 5 C. Renault 1 I. Ristorcelli G. Rocha G. Roudier 5, 6 J. Rubiño-Martín B. Rusholme M. Sandri D. Santos 1 G. Savini D. Scott D. Soler D. Spencer V. Stolyarov R. Sudiwala R. Sunyaev D. Sutton A. Suur-Uski J. Sygnet J. Tauber L. Terenzi L. Toffolatti M. Tomasi M. Tristram 7 M. Tucci 7 G. Umana L. Valenziano J. Valiviita B. van Tent 11 P. Vielva Francesca Villa A. Wade D. Wandelt K. Wehus H. Wiesemeyer D. Yvon 10 A. Zacchei A. Zonca
1 LPSC - Laboratoire de Physique Subatomique et de Cosmologie
2 IAS - Institut d'astrophysique spatiale
3 IAP - Institut d'Astrophysique de Paris
4 IRAP - Institut de recherche en astrophysique et planétologie
5 APC (UMR_7164) - AstroParticule et Cosmologie
6 LERMA - Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique
7 LAL - Laboratoire de l'Accélérateur Linéaire
8 LAM - Laboratoire d'Astrophysique de Marseille
9 AIM (UMR_7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
10 IRFU - Institut de Recherches sur les lois Fondamentales de l'Univers
11 LPT - Laboratoire de Physique Théorique d'Orsay [Orsay]
Abstract : The role of the magnetic field in the formation of the filamentary structures observed in the interstellar medium (ISM) is a debated topic. The Planck all-sky maps of linearly polarized emission from dust at 353GHz provide the required combination of imaging and statistics to study the correlation between the structures of the Galactic magnetic field and of interstellar matter, both in the diffuse ISM and in molecular clouds. The data reveal structures, or ridges, in the intensity map with counterparts in the Stokes Q and/or U maps. We focus on structures at intermediate and high Galactic latitudes with column density from 1020 to 1022 cm−2. We measure the magnetic field orientation on the plane of the sky from the polarization data, and present an algorithm to estimate the orientation of the ridges from the dust intensity map. We use analytical models to account for projection effects. Comparing polarization angles on and off the structures, we estimate the mean ratio between the strengths of the turbulent and mean components of the magnetic field to be between 0.6 and 1.0, with a preferred value of 0.8. We find that the ridges are preferentially aligned with the magnetic field measured on the structures. This trend becomes more striking for increasing polarization fraction and decreasing column density. We interpret the increase of alignment with polarization fraction as a consequence of projections effects. The decrease of alignment for high column density is not due to a loss of correlation between the structures and the geometry of the magnetic field. In molecular complexes, we observe structures perpendicular to the magnetic field, which cannot be accounted for by projection effects. We discuss our results in the context of models and MHD simulations, which describe the formation of structures in the magnetized ISM.
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Contributor : Vincent Guillet Connect in order to contact the contributor
Submitted on : Tuesday, January 18, 2022 - 5:03:40 PM
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INSU | SU-SCIENCES | USPC | UNIV-PARIS7 | OMP-IRAP | IAP | LAM | IRFU-APC | LERMA | UNIV-PARIS | INSTITUT-SCIENCES-LUMIERE | IRFU-AIM | APC | SU-TI | METEO | PSL | UP-SCIENCES | UNIV-CERGY | CEA | CEA-UPSAY | OBSPM | UNIV-AMU | OSU-INSTITUT-PYTHEAS | UNIV-PARIS-SACLAY | SORBONNE-UNIVERSITE | CNRS | UNIV-TLSE3 | UGA | CEA-DRF | CAPSANTE | DSM-IRFU | IN2P3 | LPSC | LAL | OMP | UPMC | IRD

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Planck Collaboration, R. Adam, R. Ade, N. Aghanim, R. Alves, et al.. Planck intermediate results. XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust. Astronomy and Astrophysics - A&A, EDP Sciences, 2016, 586, pp.A135. ⟨10.1051/0004-6361/201425044⟩. ⟨hal-02022197⟩

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