Use este identificador para citar o ir al link de este elemento: http://hdl.handle.net/1843/60212
Tipo: Artigo de Periódico
Título: Magnetic field morphology in nearby molecular clouds as revealed by starlight and submillimetre polarization
Autor(es): Juan Diego Soler
Peter Gordon Martin
Marc-Antoine Miville-Deschênes
Felipe de Oliveira Alves
François Boulanger
Andrea Bracco
Edith Falgarone
Gabriel Armando Pellegatti Franco
Vincent Guillet
Patrick Hennebelle
François Levrier
Resumen: Within four nearby (d < 160 pc) molecular clouds, we statistically evaluated the structure of the interstellar magnetic field, projected on the plane of the sky and integrated along the line of sight, as inferred from the polarized thermal emission of Galactic dust observed by Planck at 353 GHz and from the optical and near-infrared polarization of background starlight. We compared the dispersion of the field orientation directly in vicinities with an area equivalent to that subtended by the Planck effective beam at 353 GHz (10′) and using the second-order structure functions of the field orientation angles. We found that the average dispersion of the starlight-inferred field orientations within 10′-diameter vicinities is less than 20°, and that at these scales the mean field orientation is on average within 5° of that inferred from the submillimetre polarization observations in the considered regions. We also found that the dispersion of starlight polarization orientations and the polarization fractions within these vicinities are well reproduced by a Gaussian model of the turbulent structure of the magnetic field, in agreement with the findings reported by the Planck Collaboration at scales ℓ > 10′ and for comparable column densities. At scales ℓ > 10′, we found differences of up to 14.̊7 between the second-order structure functions obtained from starlight and submillimetre polarization observations in the same positions in the plane of the sky, but comparison with a Gaussian model of the turbulent structure of the magnetic field indicates that these differences are small and are consistent with the difference in angular resolution between both techniques. The differences between the second-order structure functions calculated with each technique suggests that the increase in the angular resolution obtained with the starlight polarization observations does not introduce significant corrections to the dispersion of polarization orientations used in the calculation of the molecular-cloud-scale magnetic field strengths reported in previous studies by the Planck Collaboration.
Asunto: Campos magnéticos
Polarimetria
Nuvens moleculares
Idioma: eng
País: Brasil
Editor: Universidade Federal de Minas Gerais
Sigla da Institución: UFMG
Departamento: ICX - DEPARTAMENTO DE FÍSICA
Tipo de acceso: Acesso Aberto
Identificador DOI: https://doi.org/10.1051/0004-6361/201628996
URI: http://hdl.handle.net/1843/60212
Fecha del documento: 2016
metadata.dc.url.externa: https://www.aanda.org/articles/aa/abs/2016/12/aa28996-16/aa28996-16.html
metadata.dc.relation.ispartof: Astronomy & Astrophysics
Aparece en las colecciones:Artigo de Periódico

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