Kazan Federal University Digital Repository

Planck intermediate results: XXXIII. Signature of the magnetic field geometry of interstellar filaments in dust polarization maps

Show simple item record

dc.contributor.author Ade P.
dc.contributor.author Aghanim N.
dc.contributor.author Alves M.
dc.contributor.author Arnaud M.
dc.contributor.author Arzoumanian D.
dc.contributor.author Aumont J.
dc.contributor.author Baccigalupi C.
dc.contributor.author Banday A.
dc.contributor.author Barreiro R.
dc.contributor.author Bartolo N.
dc.contributor.author Battaner E.
dc.contributor.author Benabed K.
dc.contributor.author Benoit-Lévy A.
dc.contributor.author Bernard J.
dc.contributor.author Berné O.
dc.contributor.author Bersanelli M.
dc.contributor.author Bielewicz P.
dc.contributor.author Bonaldi A.
dc.contributor.author Bonavera L.
dc.contributor.author Bond J.
dc.contributor.author Borrill J.
dc.contributor.author Bouchet F.
dc.contributor.author Boulanger F.
dc.contributor.author Bracco A.
dc.contributor.author Burigana C.
dc.contributor.author Calabrese E.
dc.contributor.author Cardoso J.
dc.contributor.author Catalano A.
dc.contributor.author Chamballu A.
dc.contributor.author Chiang H.
dc.contributor.author Christensen P.
dc.contributor.author Clements D.
dc.contributor.author Colombi S.
dc.contributor.author Colombo L.
dc.contributor.author Combet C.
dc.contributor.author Couchot F.
dc.contributor.author Crill B.
dc.contributor.author Curto A.
dc.contributor.author Cuttaia F.
dc.contributor.author Danese L.
dc.contributor.author Davies R.
dc.contributor.author Davis R.
dc.contributor.author De Bernardis P.
dc.contributor.author De Rosa A.
dc.contributor.author De Zotti G.
dc.contributor.author Delabrouille J.
dc.contributor.author Dickinson C.
dc.contributor.author Diego J.
dc.contributor.author Donzelli S.
dc.contributor.author Doré O.
dc.contributor.author Douspis M.
dc.contributor.author Ducout A.
dc.contributor.author Dupac X.
dc.contributor.author Elsner F.
dc.contributor.author Enßlin T.
dc.contributor.author Eriksen H.
dc.contributor.author Falgarone E.
dc.contributor.author Ferrière K.
dc.contributor.author Finelli F.
dc.contributor.author Forni O.
dc.contributor.author Frailis M.
dc.contributor.author Fraisse A.
dc.contributor.author Franceschi E.
dc.contributor.author Frejsel A.
dc.contributor.author Galeotta S.
dc.contributor.author Galli S.
dc.date.accessioned 2018-09-19T20:04:46Z
dc.date.available 2018-09-19T20:04:46Z
dc.date.issued 2016
dc.identifier.issn 0004-6361
dc.identifier.uri https://dspace.kpfu.ru/xmlui/handle/net/142519
dc.description.abstract © ESO, 2016.Planck observations at 353 GHz provide the first fully sampled maps of the polarized dust emission towards interstellar filaments and their backgrounds (i.e., the emission observed in the surroundings of the filaments). The data allow us to determine the intrinsic polarization properties of the filaments and therefore to provide insight into the structure of their magnetic field (B). We present the polarization maps of three nearby (several parsecs long) star-forming filaments of moderate column density (NH about 1022 cm-2): Musca, B211, and L1506. These three filaments are detected above the background in dust total and polarized emission. We use the spatial information to separate Stokes I, Q, and U of the filaments from those of their backgrounds, an essential step in measuring the intrinsic polarization fraction (p) and angle (ψ) of each emission component. We find that the polarization angles in the three filaments (ψfil) are coherent along their lengths and not the same as in their backgrounds (ψbg). The differences between ψfil and ψbg are 12° and 54° for Musca and L1506, respectively, and only 6° in the case of B211. These differences forMusca and L1506 are larger than the dispersions of ψ, both along the filaments and in their backgrounds. The observed changes of ψ are direct evidence of variations of the orientation of the plane of the sky (POS) projection of the magnetic field. As in previous studies, we find a decrease of several per cent in p with NH from the backgrounds to the crest of the filaments. We show that the bulk of the drop in p within the filaments cannot be explained by random fluctuations of the orientation of the magnetic field because they are too small (σψ < 10°). We recognize the degeneracy between the dust alignment efficiency (by, e.g., radiative torques) and the structure of the B-field in causing variations in p, but we argue that the decrease in p from the backgrounds to the filaments results in part from depolarization associated with the 3D structure of the B-field: both its orientation in the POS and with respect to the POS. We do not resolve the inner structure of the filaments, but at the smallest scales accessible with Planck (∼0.2 pc), the observed changes of ψ and p hold information on the magnetic field structure within filaments. They show that both the mean field and its fluctuations in the filaments are different from those of their backgrounds, which points to a coupling between the matter and the B-field in the filament formation process.
dc.relation.ispartofseries Astronomy and Astrophysics
dc.subject dust, extinction
dc.subject ISM: magnetic fields
dc.subject polarization
dc.subject submillimeter: ISM
dc.title Planck intermediate results: XXXIII. Signature of the magnetic field geometry of interstellar filaments in dust polarization maps
dc.type Article
dc.relation.ispartofseries-volume 586
dc.collection Публикации сотрудников КФУ
dc.source.id SCOPUS00046361-2016-586-SID84958949802


Files in this item

This item appears in the following Collection(s)

  • Публикации сотрудников КФУ Scopus [24551]
    Коллекция содержит публикации сотрудников Казанского федерального (до 2010 года Казанского государственного) университета, проиндексированные в БД Scopus, начиная с 1970г.

Show simple item record

Search DSpace


Advanced Search

Browse

My Account

Statistics