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We present the polarization detections in DR21(OH) from both the thermal dustemission at 1.3 mm and the CO J=2-1 line obtained with theBerkeley-Illinois-Maryland Association (BIMA) array. Our results are consistentwith the prediction of the Goldreich-Kylafis effect that the CO polarization iseither parallel or perpendicular to the magnetic field direction. The detectionof the polarized CO emission is over a more extended region than the dustpolarization, while the dust polarization provides an aide in resolving theambiguity of the CO polarization. The combined results suggest that themagnetic field direction in DR21(OH) is parallel to the CO polarization andtherefore parallel to the major axis of DR21(OH). The strong correlationbetween the CO and dust polarization suggests that magnetic fields areremarkably uniform throughout the envelope and the cores. The dispersion inpolarization position angles implies a magnetic field strength in the plane ofthe sky of about 1 mG, compared with about 0.5 mG inferred for theline-of-sight field from previous CN Zeeman observations. Our CO data also showthat both MM1 and MM2 power high-velocity outflows with $v\gtrsim$25 km/srelative to the systematic velocity.Comment: 20 pages, 7 figures, accepted for publication in Ap

Interferometric Mapping of Magnetic Fields in Star‐forming Regions. III. Dust and CO Polarization in DR 21(OH)