Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N

TL;DR

This study uses submillimeter polarization observations to analyze magnetic field structures in the massive star-forming region W75N, revealing magnetic field strength, orientation, and the influence of gravity and outflows.

Contribution

It provides detailed magnetic field measurements and insights into the role of gravity and outflows in shaping magnetic structures in W75N.

Findings

Magnetic field strength in dense cores is approximately 0.8 mG.

The region is undergoing global gravitational collapse.

Magnetic fields are influenced by gravity and outflows.

Abstract

This paper presents the results of full polarization observations of the massive star-forming region W75N, conducted with 3 arcsec spatial resolutions at 345 GHz using the Submillimeter Array (SMA). The magnetic field structures in the dense cores of the region are derived using the linearly polarized continuum emission. The overall magnetic field strength and orientation are found to agree with those from the previous observations. The plane-of-sky (POS) component of the magnetic field in the region was calculated to be 0.8 \pm 0.1 mG using the angular dispersion function (ADF) method. Further analyses involving the polarization-intensity gradient-local gravity method and H13CO+ (4-3) line data indicated that the cloud is undergoing global gravitational collapse and the magnetic field is shaped by gravity and outflows in the dense core regions.