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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/60212
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dc.creatorJuan Diego Solerpt_BR
dc.creatorPeter Gordon Martinpt_BR
dc.creatorMarc-Antoine Miville-Deschênespt_BR
dc.creatorFelipe de Oliveira Alvespt_BR
dc.creatorFrançois Boulangerpt_BR
dc.creatorAndrea Braccopt_BR
dc.creatorEdith Falgaronept_BR
dc.creatorGabriel Armando Pellegatti Francopt_BR
dc.creatorVincent Guilletpt_BR
dc.creatorPatrick Hennebellept_BR
dc.creatorFrançois Levrierpt_BR
dc.date.accessioned2023-10-30T11:57:58Z-
dc.date.available2023-10-30T11:57:58Z-
dc.date.issued2016-
dc.citation.volume596pt_BR
dc.citation.spage1pt_BR
dc.citation.epage15pt_BR
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201628996pt_BR
dc.identifier.issn1432-0746pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/60212-
dc.description.resumoWithin 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.pt_BR
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológicopt_BR
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Geraispt_BR
dc.format.mimetypepdfpt_BR
dc.languageengpt_BR
dc.publisherUniversidade Federal de Minas Geraispt_BR
dc.publisher.countryBrasilpt_BR
dc.publisher.departmentICX - DEPARTAMENTO DE FÍSICApt_BR
dc.publisher.initialsUFMGpt_BR
dc.relation.ispartofAstronomy & Astrophysics-
dc.rightsAcesso Abertopt_BR
dc.subjectMagnetic fieldspt_BR
dc.subjectMolecular cloudspt_BR
dc.subject.otherCampos magnéticospt_BR
dc.subject.otherPolarimetriapt_BR
dc.subject.otherNuvens molecularespt_BR
dc.titleMagnetic field morphology in nearby molecular clouds as revealed by starlight and submillimetre polarizationpt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://www.aanda.org/articles/aa/abs/2016/12/aa28996-16/aa28996-16.htmlpt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-0294-4465pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5236-3896pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-7351-6062pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-7945-064Xpt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-1097-6042pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-0932-3140pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-2020-2649pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-8881-3094pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-0472-7202pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-3065-9944pt_BR
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