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Cited by 88Astrophysics and Star Formation StudiesAstrophysics and Cosmic PhenomenaRadio Astronomy Observations and Technology

Polarized radio filaments outside the Galactic plane

Open access
Vidal, Matias, Dickinson, C., Davies, R. D., Leahy, J. P.·2015·Monthly Notices of the Royal Astronomical Society
DOI 10.1093/mnras/stv1328
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Abstract

We used data from the WMAP satellite at 23, 33 and 41 GHz to study the diffuse polarized emission over the entire sky. The emission originates mostly from filamentary structures with well-ordered magnetic fields. Some of these structures have been known for decades in radio continuum maps. Their origin is not clear and there are many filaments that are visible for the first time. We have identified and studied 11 filaments. The polarization fraction of some of them can be as high as 40 per cent, which is a signature of a well-ordered magnetic field. The polarization spectral indices, averaged over 18 regions in the sky is β = −3.06 ± 0.02, consistent with synchrotron radiation. There are significant variations in β over the sky (Δβ ≈ 0.2). We explore the link between the large-scale filaments and the local interstellar medium, using the model of an expanding shell in the solar vicinity. We compared observed polarization angles with the predictions from the model and found good agreement. This strongly suggests that many large-scale filaments and loops are nearby structures. This is important in the context of the Galactic magnetic field as these structures are normally included in global models, neglecting the fact that they might be local. We also studied the level of contamination added by the diffuse filaments to the CMB (cosmic microwave background) polarization power spectra. We conclude that, even though these filaments present low radio brightness, a careful removal will be necessary for future all-sky CMB polarization analysis.

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Crossref · 10.1093/mnras/stv1328

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81 of 81 references verified0 citation errors · 0 not checkable

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  • Vidal et al. found that the overall magnetic field orientation toward the sky is consistent with a magnetic shell of radius 120 pc and at a distance of 120 pc toward (320°, 5°).

    “Vidal et al. (2015) find that the overall magnetic field orientation toward the sky is consistent with a magnetic shell of radius 120 pc and at a distance of 120 pc toward (320 ◦ , 5 ◦ ) and probably represents a hot SNe bubble related to the Scorpio-Centaurus OB association (Berkhuijsen et al. 1971; Wolleben 2007; Dickinson 2018).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Vidal et al. 2015

  • Depolarization of radio emission at 2.3 GHz is clearly visible in the WMAP and Planck map at b≲30°.

    “Such depolarization is clearly visible in the 2 . 3 GHz WMAP and Planck map at b ≲ 30 ◦ (see Panel f in figure 4, and also Carretti et al. 2013; Vidal et al. 2015; Planck Collaboration et al. 2016).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Vidal et al. 2015

  • The magnetic shell found by Vidal et al. probably represents a hot SNe bubble related to the Scorpio-Centaurus OB association.

    “Vidal et al. (2015) find that the overall magnetic field orientation toward the sky is consistent with a magnetic shell of radius 120 pc and at a distance of 120 pc toward (320 ◦ , 5 ◦ ) and probably represents a hot SNe bubble related to the Scorpio-Centaurus OB association (Berkhuijsen et al. 1971; Wolleben 2007; Dickinson 2018).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Vidal et al. 2015

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Authors
Vidal, M., Dickinson, C., Davies, R. D., & Leahy, J. P.
Affiliations
University of Manchester (GB)
ORCID
Venue
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Published
2015-07-07
Volume
452
Issue
1
Pages
656-675
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
DOI
10.1093/mnras/stv1328
OpenAlex
W2145956230
Cited by
88
References
81
Citations by year
2026: 2 · 2025: 6 · 2024: 12 · 2023: 8 · 2022: 13 · 2021: 5 · 2020: 3 · 2019: 8 · 2018: 8 · 2017: 2 · 2016: 15 · 2015: 3 · 2014: 3
FWCI
5.31
Type
journal article
Language
en
Open access
Locations
  • Monthly Notices of the Royal Astronomical Society (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • Research Explorer (The University of Manchester) (submittedVersion)
  • HighWire Press Open Archive (submittedVersion)
  • arXiv (Cornell University)
Funders
Science and Technology Facilities Council (ST/F010885/1, ST/L000768/1)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
  • Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Radio Astronomy Observations and Technology
Keywords
galactic magnetic fields, synchrotron polarization, local interstellar medium, degree of polarization, cosmic microwave background

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Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.

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