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It has been proposed that the magnetic field, pervasive in the ISM, plays animportant role in the process of massive star formation. To better understandits impact at the pre and protostellar stages, high-angular resolutionobservations of polarized dust emission toward a large sample of massive densecores are needed. To this end, we used the Atacama Large Millimeter Array inBand 6 (1.3 mm) in full polarization mode to map the polarized emission fromdust grains at a physical scale of $\sim$2700 au in the massive protoclusterW43-MM1. We used these data to measure the orientation of the magnetic field atthe core scale. Then, we examined the relative orientations of the core-scalemagnetic field, of the protostellar outflows determined from CO molecular lineemission, and of the major axis of the dense cores determined from 2D Gaussianfit in the continuum emission. We found that the orientation of the dense coresis not random with respect to the magnetic field. Instead, the dense cores arecompatible with being oriented 20-50$^\deg$ with respect to the magnetic field.The outflows could be oriented 50-70$^\deg$ with respect to the magnetic field,or randomly oriented with respect to the magnetic field, similar to currentresults in low-mass star-forming regions. In conclusion, the observed alignmentof the position angle of the cores with respect to the magnetic field linesshows that the magnetic field is well coupled with the dense material; however,the 20-50$^\deg$ preferential orientation contradicts the predictions of themagnetically-controlled core-collapse models. The potential correlation of theoutflow directions with respect to the magnetic field suggests that, in somecases, the magnetic field is strong enough to control the angular momentumdistribution from the core scale down to the inner part of the circumstellardisks where outflows are triggered.

Outflows, cores and magnetic field orientations in W43-MM1 as seen by ALMA