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We present the first high-angular resolution (up to 0.7", ~5000 AU)polarization and thermal dust continuum images toward the massive star-formingregion W51 North. The observations were carried out with the SubmillimeterArray (SMA) in both the subcompact (SMA-SubC) and extended (SMA-Ext)configurations at a wavelength of 870 micron. W51 North is resolved into fourcores (SMA1 to SMA4) in the 870 micron continuum image. The associated dustpolarization exhibits more complex structures than seen at lower angularresolution. We analyze the inferred morphologies of the plane-of-sky magneticfield (B_bot) in the SMA1 to SMA4 cores and in the envelope using the SMA-Extand SMA-SubC data. These results are compared with the B_bot archive imagesobtained from the CSO and JCMT. A correlation between dust intensity gradientposition angles (phi_{nabla I}) and magnetic field position angles (phi_B) isfound in the CSO, JCMT and both SMA data sets. This correlation is furtheranalyzed quantitatively. A systematically tighter correlation betweenphi_{nabla I} and phi_B is found in the cores, whereas the correlationdecreases in outside-core regions. Magnetic field-to-gravity force ratio(Sigma_B) maps are derived using the newly developed polarization - intensitygradient method by Koch, Tang & Ho 2012. We find that the force ratios tend tobe small (Sigma_B <= 0.5) in the cores in all 4 data sets. In regions outsideof the cores, the ratios increase or the field is even dominating gravity(Sigma_B > 1). This possibly provides a physical explanation of the tighteningcorrelation between phi_{nabla I} and phi_B in the cores: the more the B fieldlines are dragged and aligned by gravity, the tighter the correlation is.Finally, we propose a schematic scenario for the magnetic field in W51 North tointerpret the four polarization observations at different physical scales.

Dust continuum and Polarization from Envelope to Cores in Star Formation: A Case Study in the W51 North region