Interferometric mapping of magnetic fields: The massive star-forming region G34.4+0.23 MM

P. C. Cortes; R. M. Crutcher; D. S. Shepherd; L. Bronfman

doi:10.1086/524355

Interferometric mapping of magnetic fields: The massive star-forming region G34.4+0.23 MM

P. C. Cortes, R. M. Crutcher, D. S. Shepherd, L. Bronfman

Astronomy

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Abstract

We report millimeter interferometric observations of polarized continuum and line emission from the massive star-forming region G34.4. Polarized thermal dust emission at 3 mm wavelength and CO J = 1 → 0 line emission were observed using the Berkeley-Illinois-Maryland Association (BIMA) array. Our results show a remarkably uniform polarization pattern in both dust and in CO J = 1 → 0 emission. In addition, the line emission presents a consistent uniform polarization pattern over most of the velocity channel maps. These uniform polarization patterns are aligned with the north-south main axis of the filament between the main millimeter source (MM) and the ultracompact H II region, which are the central sources in G34.4, suggesting a magnetic field orthogonal to this axis. This morphology is consistent with a magnetically supported disk seen roughly edge-on.

Original language	English (US)
Pages (from-to)	464-471
Number of pages	8
Journal	Astrophysical Journal
Volume	676
Issue number	1
DOIs	https://doi.org/10.1086/524355
State	Published - Mar 20 2008

Keywords

ISM: magnetic fields
Stars: formation

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Online availability

10.1086/524355

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abstract = "We report millimeter interferometric observations of polarized continuum and line emission from the massive star-forming region G34.4. Polarized thermal dust emission at 3 mm wavelength and CO J = 1 → 0 line emission were observed using the Berkeley-Illinois-Maryland Association (BIMA) array. Our results show a remarkably uniform polarization pattern in both dust and in CO J = 1 → 0 emission. In addition, the line emission presents a consistent uniform polarization pattern over most of the velocity channel maps. These uniform polarization patterns are aligned with the north-south main axis of the filament between the main millimeter source (MM) and the ultracompact H II region, which are the central sources in G34.4, suggesting a magnetic field orthogonal to this axis. This morphology is consistent with a magnetically supported disk seen roughly edge-on.",

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T1 - Interferometric mapping of magnetic fields

T2 - The massive star-forming region G34.4+0.23 MM

AU - Cortes, P. C.

AU - Crutcher, R. M.

AU - Shepherd, D. S.

AU - Bronfman, L.

PY - 2008/3/20

Y1 - 2008/3/20

N2 - We report millimeter interferometric observations of polarized continuum and line emission from the massive star-forming region G34.4. Polarized thermal dust emission at 3 mm wavelength and CO J = 1 → 0 line emission were observed using the Berkeley-Illinois-Maryland Association (BIMA) array. Our results show a remarkably uniform polarization pattern in both dust and in CO J = 1 → 0 emission. In addition, the line emission presents a consistent uniform polarization pattern over most of the velocity channel maps. These uniform polarization patterns are aligned with the north-south main axis of the filament between the main millimeter source (MM) and the ultracompact H II region, which are the central sources in G34.4, suggesting a magnetic field orthogonal to this axis. This morphology is consistent with a magnetically supported disk seen roughly edge-on.

AB - We report millimeter interferometric observations of polarized continuum and line emission from the massive star-forming region G34.4. Polarized thermal dust emission at 3 mm wavelength and CO J = 1 → 0 line emission were observed using the Berkeley-Illinois-Maryland Association (BIMA) array. Our results show a remarkably uniform polarization pattern in both dust and in CO J = 1 → 0 emission. In addition, the line emission presents a consistent uniform polarization pattern over most of the velocity channel maps. These uniform polarization patterns are aligned with the north-south main axis of the filament between the main millimeter source (MM) and the ultracompact H II region, which are the central sources in G34.4, suggesting a magnetic field orthogonal to this axis. This morphology is consistent with a magnetically supported disk seen roughly edge-on.

KW - ISM: magnetic fields

KW - Stars: formation

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Interferometric mapping of magnetic fields: The massive star-forming region G34.4+0.23 MM

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