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The role of magnetic fields during the protostellar phase of high-massstar-formation is a debated topic. In particular, it is still unclear howmagnetic fields influence the formation and dynamic of disks and outflows. Mostcurrent information on magnetic fields close to high-mass protostars comes fromH2O and OH maser observations. Recently, the first 6.7 GHz methanol maserpolarization observations were made, and they reveal strong and orderedmagnetic fields. The morphology of the magnetic field during high-massstar-formation needs to be investigated on small scales, which can only be doneusing very long baseline interferometry observations. The massive star-formingregionW75N contains three radio sources and associated masers, while alarge-scale molecular bipolar outflow is also present. Polarizationobservations of the 6.7 GHz methanol masers at high angular resolution probethe strength and structure of the magnetic field and determine its relation tothe outflow. Eight of the European VLBI network antennas were used to measurethe linear polarization and Zeeman-splitting of the 6.7 GHz methanol masers inthe star-forming region W75N. We detected 10 methanol maser features, 4 ofwhich were undetected in previous work. All arise near the source VLA1 of W75N.The linear polarization of the masers reveals a tightly ordered magnetic fieldover more than 2000 AU around VLA1 that is exactly aligned with the large-scalemolecular outflow. This is consistent with the twisted magnetic field modelproposed for explaining dust polarization observations. The Zeeman-splittingmeasured on 3 of the maser features indicates a dynamically important magneticfield in the maser region of the order of 50mG. We suggest VLA1 is the poweringsources of the bipolar outflow.

Methanol masers probing the ordered magnetic field of W75N