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

被引：0

作者：

Adam, R. ^{[68
]}

Ade, P.A.R. ^{[79
]}

Aghanim, N. ^{[54
]}

Alves, M.I.R. ^{[54
]}

Arnaud, M. ^{[66
]}

Arzoumanian, D. ^{[54
]}

Ashdown, M. ^{[6
,63
]}

Aumont, J. ^{[54
]}

Baccigalupi, C. ^{[78
]}

Banday, A.J. ^{[10
,85
]}

Barreiro, R.B. ^{[60
]}

Bartolo, N. ^{[27
]}

Battaner, E. ^{[87
,88
]}

Benabed, K. ^{[55
,84
]}

Benoit-Lévy, A. ^{[21
,55
,84
]}

Bernard, J.-P. ^{[10
,85
]}

Bersanelli, M. ^{[30
,46
]}

Bielewicz, P. ^{[10
,78
,85
]}

Bonaldi, A. ^{[62
]}

Bonavera, L. ^{[60
]}

Bond, J.R. ^{[9
]}

Borrill, J. ^{[13
,81
]}

Bouchet, F.R. ^{[55
,84
]}

Boulanger, F. ^{[54
]}

Bracco, A. ^{[54
]}

Burigana, C. ^{[28
,45
,47
]}

Butler, R.C. ^{[45
]}

Calabrese, E. ^{[83
]}

Cardoso, J.-F. ^{[1
,55
,67
]}

Catalano, A. ^{[65
,68
]}

Chamballu, A. ^{[14
,54
,66
]}

Chiang, H.C. ^{[7
,24
]}

Christensen, P.R. ^{[33
,75
]}

Colombi, S. ^{[55
,84
]}

Colombo, L.P.L. ^{[20
,61
]}

Combet, C. ^{[68
]}

Couchot, F. ^{[64
]}

Crill, B.P. ^{[61
,76
]}

Curto, A. ^{[6
,60
]}

Cuttaia, F. ^{[45
]}

Danese, L. ^{[78
]}

Davies, R.D. ^{[62
]}

Davis, R.J. ^{[62
]}

De Bernardis, P. ^{[29
]}

De Rosa, A. ^{[45
]}

De Zotti, G. ^{[42
,78
]}

Delabrouille, J. ^{[1
]}

Dickinson, C. ^{[62
]}

Diego, J.M. ^{[60
]}

Dole, H. ^{[53
,54
]}

机构：

[1] APC, AstroParticule et Cosmologie, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Université Paris Diderot, 10, Rue Alice Domon et Ĺeonie Duquet, Sorbonne Paris Cité, Paris Cedex 13,75205, France

[2] African Institute for Mathematical Sciences, 6-8 Melrose Road, Muizenberg, Cape Town, South Africa

[3] Agenzia Spaziale Italiana Science Data Center, Via del Politecnico snc, Rome,00133, Italy

[4] Agenzia Spaziale Italiana, Viale Liegi 26, Rome, Italy

[5] LAM (Laboratoire D'Astrophysique de Marseille) UMR 7326, Aix Marseille Université, CNRS, Marseille,13388, France

[6] Cavendish Laboratory, Astrophysics Group, University of Cambridge, J J Thomson Avenue, Cambridge,CB3 0HE, United Kingdom

[7] Astrophysics and Cosmology Research Unit, Statistics and Computer Science, University of KwaZulu-Natal, Westville Campus, Private BagX54001, Durban,4000, South Africa

[8] Atacama Large Millimeter/submillimeter Array, ALMA Santiago Central Offces, Alonso de Cordova 3107, Vitacura, Casilla, Santiago,763 0355, Chile

[9] CITA, University of Toronto, 60 St. George St., Toronto,ON,M5S3H8, Canada

[10] CNRS, IRAP, 9 Av. colonel Roche, BP 44346, Toulouse Cedex 4,F-31028, France

[11] California Institute of Technology, Pasadena,CA, United States

[12] Centro de Estudios de Física del Cosmos de Araoǵn (CEFCA), Plaza San Juan, 1, planta 2, Teruel,E-44001, Spain

[13] Lawrence Berkeley National Laboratory, Computational Cosmology Center, Berkeley,CA, United States

[14] DSM/Irfu/SPP, CEA-Saclay, Gif-sur-Yvette Cedex,F-91191, France

[15] DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, Kgs. Lyngby,DK-2800, Denmark

[16] Département de Physique Théorique, Université de Genéve, 24, Quai E. Ansermet, Genéve 4,1211, Switzerland

[17] Departamento de Física, Universidad de Oviedo, Avda. Calvo Sotelo s/n, Oviedo, Spain

[18] Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, GL Nijmegen,6500, Netherlands

[19] Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver,BC, Canada

[20] Department of Physics and Astronomy, Dana and David Dornsife College of Letter, Arts and Sciences, University of Southern California, Los Angeles,CA,90089, United States

[21] Department of Physics and Astronomy, University College London, London,WC1E 6BT, United Kingdom

[22] Department of Physics, Keen Physics Building, Florida State University, 77 Chieftan Way, Tallahassee,FL, United States

[23] Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2a, Helsinki, Finland

[24] Department of Physics, Princeton University, Princeton,NJ, United States

[25] Department of Physics, University of California, Santa Barbara,CA, United States

[26] Department of Physics, University of Illinois at Urbana-Champaign, 1110 West Green Street, Urbana,IL, United States

[27] Dipartimento di Fisica E Astronomia G. Galilei, Universitá degli Studi di Padova, via Marzolo 8, Padova,35131, Italy

[28] Dipartimento di Fisica E Scienze della Terra, Universitá di Ferrara, Via Saragat 1, Ferrara,44122, Italy

[29] Dipartimento di Fisica, Universitá La Sapienza, P. le A. Moro 2, Rome, Italy

[30] Dipartimento di Fisica, Universitá degli Studi di Milano, Via Celoria, 16, Milan, Italy

[31] Dipartimento di Fisica, Universitá degli Studi di Trieste, via A. Valerio 2, Trieste, Italy

[32] Dipartimento di Fisica, Universitá di Roma Tor Vergata, via della Ricerca Scientifica, 1, Rome, Italy

[33] Discovery Center, Niels Bohr Institute, Blegdamsvej 17, Copenhagen, Denmark

[34] Dpto. Astrofísica, Universidad de la Laguna (ULL), La Laguna, Tenerife,E-38206, Spain

[35] European Southern Observatory, ESO Vitacura, Alonso de Cordova 3107, Vitacura, Casilla, Santiago,19001, Chile

[36] European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Madrid, Villanueva de la Cañada, Spain

[37] European Space Agency, ESTEC, Keplerlaan 1, Noordwijk,AZ,2201, Netherlands

[38] Facoltá di Ingegneria, Universita degli Studi E-Campus, Via Isimbardi 10, Novedrate,CO,22060, Italy

[39] Theoretical Physics Department, HGSFP and University of Heidelberg, Philosophenweg 16, Heidelberg,69120, Germany

[40] Helsinki Institute of Physics, University of Helsinki, Gustaf Hällströmin katu 2, Helsinki, Finland

[41] INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78, Catania, Italy

[42] INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, Italy

[43] INAF - Osservatorio Astronomico di Roma, via di Frascati 33, Monte Porzio Catone, Italy

[44] INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, Trieste, Italy

[45] INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy

[46] INAF/IASF Milano, Via E. Bassini 15, Milan, Italy

[47] INFN, Sezione di Bologna, Via Irnerio 46, Bologna,I-40126, Italy

[48] INFN, Sezione di Roma 1, Università di Roma Sapienza, Piazzale Aldo Moro 2, Rome,00185, Italy

[49] INFN/National Institute for Nuclear Physics, Via Valerio 2, Trieste,I-34127, Italy

[50] IPAG: Institut de Planétologie et d'Astrophysique de Grenoble, CNRS, IPAG, Université Grenoble Alpes, IPAG, Grenoble,F-38000, France

来源：

Astronomy and Astrophysics | 2016年 / 586卷

关键词：

Filamentary structures - Galactic magnetic fields - ISM : clouds - ISM: magnetic fields - ISM: structure - Linearly polarized emission - Magnetic field orientations - Polarization fractions;

D O I：

暂无

中图分类号：

学科分类号：

摘要：

The role of the magnetic field in the formation of the filamentary structures observed in the interstellar medium (ISM) is a debated topic owing to the paucity of relevant observations needed to test existing models. The Planck all-sky maps of linearly polarized emission from dust at 353 GHz provide the required combination of imaging and statistics to study the correlation between the structures of the Galactic magnetic field and of interstellar matter over the whole sky, both in the diffuse ISM and in molecular clouds. The data reveal that structures, or ridges, in the intensity map have counterparts in the Stokes Q and/or U maps. We focus our study on structures at intermediate and high Galactic latitudes, which cover two orders of magnitude in column density, from 1020 to 1022 cm2. 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 o 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 usually aligned with the magnetic field measured on the structures. This statistical trend becomes more striking for increasing polarization fraction and decreasing column density. There is no alignment for the highest column density ridges. We interpret the increase in alignment with polarization fraction as a consequence of projection effects. We present maps to show that the decrease in alignment for high column density is not due to a loss of correlation between the distribution of matter and the geometry of the magnetic field. In molecular complexes, we also observe structures perpendicular to the magnetic field, which, statistically, cannot be accounted for by projection effects. This first statistical study of the relative orientation between the matter structures and the magnetic field in the ISM points out that, at the angular scales probed by Planck, the field geometry projected on the plane of the sky is correlated with the distribution of matter. In the diffuse ISM, the structures of matter are usually aligned with the magnetic field, while perpendicular structures appear in molecular clouds. We discuss our results in the context of models and MHD simulations, which attempt to describe the respective roles of turbulence, magnetic field, and self-gravity in the formation of structures in the magnetized ISM.

引用

页码：1 / 25

共 7 条

[1] Planck intermediate results XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust
Adam, R.
Ade, P. A. R.
Aghanim, N.
Alves, M. I. R.
Arnaud, M.
Arzoumanian, D.
Ashdown, M.
Aumont, J.
Baccigalupi, C.
Banday, A. J.
Barreiro, R. B.
Bartolo, N.
Battaner, E.
Benabed, K.
Benoit-Levy, 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.
Butler, R. C.
Calabrese, E.
Cardoso, J-F
Catalano, A.
Chamballu, A.
Chiang, H. C.
Christensen, P. R.
Colombi, S.
Colombo, L. P. L.
Combet, C.
Couchot, F.
Crill, B. P.
Curto, A.
Cuttaia, F.
Danese, L.
Davies, R. D.
Davis, R. J.
de Bernardis, P.
de Rosa, A.
de Zotti, G.
Delabrouillel, J.
Dickinson, C.
Diego, J. M.
Dole, H.
ASTRONOMY & ASTROPHYSICS, 2016, 586
[2] Planck intermediate results XXXIII. Signature of the magnetic field geometry of interstellar filaments in dust polarization maps
Ade, P. A. R.
Aghanim, N.
Alves, M. I. R.
Arnaud, M.
Arzoumanian, D.
Aumont, J.
Baccigalupi, C.
Banday, A. J.
Barreiro, R. B.
Bartolo, N.
Battaner, E.
Benabed, K.
Benoit-Levy, A.
Bernard, J-P.
Berne, O.
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.
Chiang, H. C.
Christensen, P. R.
Clements, D. L.
Colombi, S.
Colombo, L. P. L.
Combet, C.
Couchot, F.
Crill, B. P.
Curto, A.
Cuttaia, F.
Danese, L.
Davies, R. D.
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[3] Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible
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ASTRONOMY & ASTROPHYSICS, 2015, 576
[4] Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible
20151600767858
Guillet, V. (vincent.guillet@ias.u-psud.fr), 1600, EDP Sciences (576):
[5] Planck intermediate results XLIV. Structure of the Galactic magnetic field from dust polarization maps of the southern Galactic cap
Aghanim, N.
Alves, M. I. R.
Arzoumanian, D.
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ASTRONOMY & ASTROPHYSICS, 2016, 596
[6] What are we learning from the relative orientation between density structures and the magnetic field in molecular clouds?
Soler, J. D.
Hennebelle, P.
ASTRONOMY & ASTROPHYSICS, 2017, 607
[7] The relative orientation between the magnetic field and gas density structures in non-gravitating turbulent media
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Soler, Juan D.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2020, 499 (04) : 4785 - 4792

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