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Magnetic fields are dynamically important at all scales of protostellar collapse, and they can both aid and hinder this process depending on the field strength and orientation. On large scales the field can direct the flow of material, and on small scales it can prevent large disks from growing in the youngest protostars. However, at some point during the star formation process, the field becomes decoupled from the infalling material. The time and spatial scales of this decoupling is not yet known and polarization observations that probe the spatial scales necessary to determine when this occurs are lacking. In this talk I will present multi-scale, multi-wavelength polarization observations of the Bok globule L483. The projected field orientation in L483 is seen to be consistent from core down to outer envelope scales, suggesting that the collapse on these scales is magnetically regulated. However, on smaller, inner envelope (1000 au) scales, the field is observed to be twisted. This twisted field is observed to be approximately perpendicular to the dust continuum envelope observed, suggesting that the field might still be regulating the collapse at these smaller scales. High-resolution ALMA observations of L483 reveal that it is forming a close binary, and we believe this twisted field morphology could be the result of the migrating stars. If this is the case, then we may be able to use the magnetic field morphology to infer how a binary system formed.