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IRAS20126+4104 is a well studied B0.5 protostar that is surrounded by a ~1000au Keplerian disk and is where a large-scale outflow originates. Both 6.7-GHzCH3OH masers and 22-GHz H2O masers have been detected toward this young stellarobject. The CH3OH masers trace the Keplerian disk, while the H2O masers areassociated with the surface of the conical jet. Recently, observations of dustpolarized emission (350 um) at an angular resolution of 9 arcseconds (~15000au) have revealed an S-shaped morphology of the magnetic field aroundIRAS20126+4104. The observations of polarized maser emissions at milliarcsecondresolution (~20 au) can make a crucial contribution to understanding theorientation of the magnetic field close to IRAS20126+4104. This will allow usto determine whether the magnetic field morphology changes from arcsecondresolution to milliarcsecond resolution. The European VLBI Network was used tomeasure the linear polarization and the Zeeman splitting of the 6.7-GHz CH3OHmasers toward IRAS20126+4104. The NRAO Very Long Baseline Array was used tomeasure the linear polarization and the Zeeman splitting of the 22-GHz H2Omasers toward the same region. We detected 26 CH3OH masers and 5 H2O masers athigh angular resolution. Linear polarization emission was observed toward threeCH3OH masers and toward one H2O maser. Significant Zeeman splitting wasmeasured in one CH3OH maser (\Delta V_{Z}=-9.2 +/- 1.4 m/s). No significant (5sigma) magnetic field strength was measured using the H2O masers. We found thatin IRAS20126+4104 the rotational energy is less than the magnetic energy.

The magnetic field at milliarcsecond resolution around IRAS20126+4104