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The magnetic field is a key ingredient in the recipe of star formation. Overthe past two decades, millimeter and submillimeter interferometers have mademajor strides in unveiling the role of the magnetic field in star formation atprogressively smaller spatial scales. From the kiloparsec scale of molecularclouds down to the inner few hundred au immediately surrounding forming stars,the polarization at millimeter and submillimeter wavelengths is dominated bypolarized thermal dust emission, where the dust grains are aligned relative tothe magnetic field. Interferometric studies have focused on this dustpolarization and occasionally on the polarization of spectral-line emission. Wereview the current state of the field of magnetized star formation in thecontext of several questions that continue to motivate the studies of high- andlow-mass star formation. By aggregating and analyzing the results fromindividual studies, we come to several conclusions: (1) Magnetic fields andoutflows from low-mass protostellar cores are randomly aligned, suggesting thatthe magnetic field at ~1000 au scales is not the dominant factor in setting theangular momentum of embedded disks and outflows. (2) Recent measurements of thethermal and dynamic properties in high-mass star-forming regions reveal smallvirial parameters, challenging the assumption of equilibrium star formation.However, we estimate that a magnetic field strength of a fraction of a mG toseveral mG in these objects could bring the dense gas close to a state ofequilibrium. Finally, (3) We find that the small number of sources withhourglass-shaped magnetic field morphologies at 0.01 -- 0.1 pc scales cannot beexplained purely by projection effects, suggesting that while it does occuroccasionally, magnetically dominated core collapse is not the predominant modeof low- or high-mass star formation. [Abridged]

Interferometric observations of magnetic fields in forming stars