ALMA High Angular Resolution Polarization Study; An Extremely Young Class 0 Source, OMC-3/MMS 6

Abstract

Using the $\approx$15km ALMA long baselines, we imaged the Stokes $I$ emission and linearly polarized intensity ($PI$) in the 1.1-mm continuum band of a very young intermediate-mass protostellar source, MMS 6, in the Orion Molecular Cloud-3. The achieved angular resolution, $0^{\prime \prime }.02\times 0^{\prime \prime }.03$ ($\approx$10 AU), shows for the first time a wealth of data on the dust emission polarization in the central 200 AU of a protostar. The $PI$ peak is offset to the south-west (SW) by $\approx$20 AU with respect to the Stokes $I$ peak. Its polarization degree is 11 % with its $E$-vector orientation of P.A.$\approx 135^{\circ }$. A partial ring-like structure with a radius of $\approx$80 AU is detected in $PI$ but not in the Stokes $I$. NW (north-west) and SE (south-east) parts of the ring are bright with a high polarization degree of $\gtrsim$10 %, and their $E$-vector orientations are roughly orthogonal to those observed near the center. We also detected arm-like polarized structures, extending to 1000 AU scale to the north, with the $E$-vectors aligned along the minor axis of the structures. We explored possible origins of the polarized emission comparing with magnetohydrodynamical (MHD) simulations of the toroidal wrapping of the magnetic field. The simulations are consistent with the $PI$ emission in the ring-like and the extended arm-like structures observed with ALMA. However, the current simulations do not completely reproduce observed polarization characteristics in the central 50 AU. Although the self-scattering model can explain the polarization pattern and positional offset between the Stokes $I$ and $PI$, this model is not able to reproduce the observed high degree of polarization.

47 pages, 9 figures, 4 tables, Accepted for publication in ApJ

References in corpus (14)

• The distance to the Orion Nebula
• Tracing Magnetic Fields with Aligned Grains
• Magnetic Fields in the Formation of Sun-Like Stars
• Magnetic Braking and Protostellar Disk Formation: The Ideal MHD Limit
• The Gould's Belt Distances Survey (GOBELINS) II. Distances and structure towards the Orion Molecular Clouds
• Magnetic Fields and Massive Star Formation
• The evidence of radio polarization induced by the radiative grain alignment and self-scattering of dust grains in a protoplanetary disk
• ALMA Reveals Transition of Polarization Pattern with Wavelength in HL Tau's Disk
• Submillimeter polarization observation of the protoplanetary disk around HD 142527
• Grand Design Spiral Arms in A Young Forming Circumstellar Disk
• Subsonic Mechanical Alignment of Irregular Grains
• ALMA observations of dust polarization and molecular line emission from the Class 0 protostellar source Serpens SMM1
• Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
• On the Role of Pseudodisk Warping and Reconnection in Protostellar Disk Formation in Turbulent Magnetized Cores

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