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Planck intermediate results XXXIV. The magnetic field structure in the Rosette Nebula

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Title: Planck intermediate results XXXIV. The magnetic field structure in the Rosette Nebula
Authors: Aghanim, N
Alves, MIR
Arnaud, M
Arzoumanian, D
Aumont, J
Baccigalupi, C
Banday, AJ
Barreiro, RB
Bartolo, N
Battaner, E
Benabed, K
Benoit-Levy, A
Bernard, J-P
Bersanelli, M
Bielewicz, P
Bonaldi, A
Bonavera, L
Bond, JR
Borrill, J
Bouchet, FR
Boulanger, F
Bracco, A
Burigana, C
Calabrese, E
Cardoso, J-F
Catalano, A
Chamballu, A
Chiang, HC
Christensen, PR
Colombi, S
Colombo, LPL
Combet, C
Couchot, F
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
Dole, H
Donzelli, S
Dore, O
Douspis, M
Ducout, A
Dupac, X
Efstathiou, G
Elsner, F
Ensslin, TA
Eriksen, HK
Falgarone, E
Ferriere, K
Finelli, F
Forni, O
Frailis, M
Fraisse, AA
Franceschi, E
Frejsel, A
Galeotta, S
Galli, S
Ganga, K
Ghosh, T
Giard, M
Gjerlow, E
Gonzalez-Nuevo, J
Gorski, KM
Gregorio, A
Gruppuso, A
Guillet, V
Hansen, FK
Hanson, D
Harrison, DL
Henrot-Versille, S
Herranz, D
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hornstrup, A
Hovest, W
Huffenberger, KM
Hurier, G
Jaffe, AH
Jaffe, TR
Jewell, J
Juvela, M
Keskitalo, R
Kisner, TS
Knoche, J
Kunz, M
Kurki-Suonio, H
Lagache, G
Lamarre, J-M
Lasenby, A
Lattanzi, M
Lawrence, CR
Leonardi, R
Levrier, F
Liguori, M
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Macias-Perez, JF
Maffei, B
Maino, D
Mandolesi, N
Mangilli, A
Maris, M
Martin, PG
Martinez-Gonzalez, E
Masi, S
Matarrese, S
Melchiorri, A
Mendes, L
Mennella, A
Migliaccio, M
Miville-Deschenes, M-A
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Moss, A
Munshi, D
Murphy, JA
Naselsky, P
Nati, F
Natoli, P
Netterfield, CB
Noviello, F
Novikov, D
Novikov, I
Oppermann, N
Pagano, L
Pajot, F
Paladini, R
Paoletti, D
Pasian, F
Patanchon, G
Perdereau, O
Pettorino, V
Piacentini, F
Piat, M
Pietrobon, D
Plaszczynski, S
Pointecouteau, E
Polenta, G
Ponthieu, N
Pratt, GW
Prezeau, G
Prunet, S
Puget, J-L
Rebolo, R
Reinecke, M
Remazeilles, M
Renault, C
Renzi, A
Ristorcelli, I
Rocha, G
Rosset, C
Rossetti, M
Roudier, G
Rubino-Martin, JA
Rusholme, B
Sandri, M
Santos, D
Savelainen, M
Savini, G
Scott, D
Soler, JD
Spencer, LD
Stolyarov, V
Sutton, D
Suur-Uski, A-S
Sygnet, J-F
Tauber, JA
Terenzi, L
Toffolatti, L
Tomasi, M
Tristram, M
Tucci, M
Tuovinen, J
Valenziano, L
Valiviita, J
Van Tent, B
Vielva, P
Villa, F
Wade, LA
Wandelt, BD
Wehus, IK
Wiesemeyer, H
Yvon, D
Zacchei, A
Zonca, A
Item Type: Journal Article
Abstract: Planck has mapped the polarized dust emission over the whole sky, making it possible to trace the Galactic magnetic field structure that pervades the interstellar medium (ISM). We combine polarization data from Planck with rotation measure (RM) observations towards a massive star-forming region, the Rosette Nebula in the Monoceros molecular cloud, to study its magnetic field structure and the impact of an expanding H ii region on the morphology of the field. We derive an analytical solution for the magnetic field, assumed to evolve from an initially uniform configuration following the expansion of ionized gas and the formation of a shell of swept-up ISM. From the RM data we estimate a mean value of the line-of-sight component of the magnetic field of about 3 μG (towards the observer) in the Rosette Nebula, for a uniform electron density of about 12 cm-3. The dust shell that surrounds the Rosette H ii region is clearly observed in the Planck intensity map at 353 GHz, with a polarization signal significantly different from that of the local background when considered asa whole. The Planck observations constrain the plane-of-the-sky orientation of the magnetic field in the Rosette’s parent molecular cloud to be mostly aligned with the large-scale field along the Galactic plane. The Planck data are compared with the analytical model, which predicts the mean polarization properties of a spherical and uniform dust shell for a given orientation of the field. This comparison leads to an upper limit of about 45° on the angle between the line of sight and the magnetic field in the Rosette complex, for an assumed intrinsic dust polarization fraction of 4%. This field direction can reproduce the RM values detected in the ionized region if the magnetic field strength in the Monoceros molecular cloud is in the range 6.5–9 μG. The present analytical model is able to reproduce the RM distribution across the ionized nebula, as well as the mean dust polarization properties of the swept-up shell, and can be directly applied to other similar objects.
Issue Date: 9-Feb-2016
Date of Acceptance: 8-Apr-2015
URI: http://hdl.handle.net/10044/1/44009
DOI: http://dx.doi.org/10.1051/0004-6361/201525616
ISSN: 1432-0746
Publisher: EDP SCIENCES
Journal / Book Title: ASTRONOMY & ASTROPHYSICS
Volume: 586
Copyright Statement: © 2016 ESO
Sponsor/Funder: Science and Technology Facilities Council (STFC)
Science and Technology Facilities Council (STFC)
Science and Technology Facilities Council (STFC)
Science and Technology Facilities Council (STFC)
Science and Technology Facilities Council (STFC)
Funder's Grant Number: ST/H001239/1
ST/J001368/1
ST/K001051/1
ST/K004131/1
ST/N001206/1
Keywords: Science & Technology
Physical Sciences
Astronomy & Astrophysics
ISM: magnetic fields
polarization
radiation mechanisms: general
radio continuum: ISM
submillimeter: ISM
H-II REGIONS
MOLECULAR CLOUDS
STAR-FORMATION
FARADAY-ROTATION
STOKES PARAMETERS
ELEPHANT-TRUNK
GALACTIC PLANE
HII-REGIONS
NGC 2244
EMISSION
astro-ph.GA
astro-ph.GA
Astronomy & Astrophysics
0201 Astronomical And Space Sciences
Publication Status: Published
Article Number: ARTN A137
Appears in Collections:Physics
Astrophysics
Faculty of Natural Sciences



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