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Context. Submillimeter Array (SMA) 870 micron polarization observations ofthe hot molecular core G31.41+0.31 revealed one of the clearest examples up todate of an hourglass-shaped magnetic field morphology in a high-massstar-forming region. Aims. To better establish the role that the magnetic fieldplays in the collapse of G31.41+0.31, we carried out Atacama LargeMillimeter/submillimeter Array (ALMA) observations of the polarized dustcontinuum emission at 1.3 mm with an angular resolution four times higher thanthat of the previous (sub)millimeter observations to achieve an unprecedentedimage of the magnetic field morphology. Methods. We used ALMA to perform fullpolarization observations at 233 GHz (Band 6). The resulting synthesized beamis 0.28"x0"20 which, at the distance of the source, corresponds to a spatialresolution of ~875 au. Results. The observations resolve the structure of themagnetic field in G31.41+0.31 and allow us to study the field in detail. Thepolarized emission in the Main core of G31.41+0.41is successfully fit with asemi-analytical magnetostatic model of a toroid supported by magnetic fields.The best fit model suggests that the magnetic field is well represented by apoloidal field with a possible contribution of a toroidal component of ~10% ofthe poloidal component, oriented southeast to northwest at ~ -44 deg and withan inclination of ~-45 degr. The magnetic field is oriented perpendicular tothe northeast to southwest velocity gradient detected in this core on scalesfrom 1E3-1E4 au. This supports the hypothesis that the velocity gradient is dueto rotation and suggests that such a rotation has little effect on the magneticfield. The strength of the magnetic field estimated in the central region ofthe core with the Davis-Chandrasekhar-Fermi method is ~8-13 mG and implies thatthe mass-to-flux ratio in this region is slightly supercritical ...

ALMA resolves the hourglass magnetic field in G31.41+0.31