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The role of the magnetic field during protostellar collapse is poorlyconstrained from an observational point of view, although it could besignificant if we believe state-of-the-art models of protostellar formation. Wepresent polarimetric observations of the 233 GHz thermal dust continuumemission obtained with ALMA in the B335 Class 0 protostar. Linearly polarizeddust emission arising from the circumstellar material in the envelope of B335is detected at all scales probed by our observations, from radii of 50 to 1000au. The magnetic field structure producing the dust polarization has a veryordered topology in the inner envelope, with a transition from a large-scalepoloidal magnetic field, in the outflow direction, to strongly pinched in theequatorial direction. This is probably due to magnetic field lines beingdragged along the dominating infall direction since B335 does not exhibitprominent rotation. Our data and their qualitative comparison to a family ofmagnetized protostellar collapse models show that, during the magnetizedcollapse in B335, the magnetic field is maintaining a high level oforganization from scales 1000 au to 50 au: this suggests the field isdynamically relevant and capable of influencing the typical outcome ofprotostellar collapse, such as regulating the disk size in B335.

Magnetically regulated collapse in the B335 protostar ? I. ALMA observations of the polarized dust emission