Interferometric Mapping of Magnetic fields: NGC2071IR

Abstract

We present polarization maps of NGC2071IR from thermal dust emission at 1.3 mm and from CO J=$2\to 1$ line emission. The observations were obtained using the Berkeley-Illinois-Maryland Association array in the period 2002-2004. We detected dust and line polarized emission from NGC2071IR that we used to constrain the morphology of the magnetic field. From CO J=$2\to 1$ polarized emission we found evidence for a magnetic field in the powerful bipolar outflow present in this region. We calculated a visual extinction $A_{\mathrm{v}}\approx 26$ mag from our dust observations. This result, when compared with early single dish work, seems to show that dust grains emit polarized radiation efficiently at higher densities than previously thought. Mechanical alignment by the outflow is proposed to explain the polarization pattern observed in NGC2071IR, which is consistent with the observed flattening in this source.

17 pages, 4 Figures, Accepted for publication in ApJ

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• Evolution of Magnetic Fields in High Mass Star Formation: SMA dust polarization image of the UCHII region G5.89-0.39
• Helical Magnetic Fields in the NGC1333 IRAS 4A Protostellar Outflows
• Multiplicity, Disks and Jets in the NGC 2071 Star-Forming Region
• Interferometric Mapping of Magnetic Fields: The massive star forming region G34.4+0.23 MM
• The JCMT BISTRO Survey: An 850/450$\mu$m Polarization Study of NGC 2071IR in OrionB
• Low Level Carbon Monoxide Line Polarization in two Protoplanetary Disks: HD 142527 and IM Lup
• The Mechanical Alignment of Dust (MAD) I: On the spin-up process of fractal grains by a gas-dust drift
• Observations of the Goldreich-Kylafis effect in star-forming regions with XPOL at the IRAM 30m telescope
• Tracing the large-scale magnetic field morphology in protoplanetary disks using molecular line polarization
• Discs and outflows in the early phases of massive star formation: influence of magnetic fields and ambipolar diffusion