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The combination of dispersion analysis from FIR polarimetry and the Davis-Chandrasekhar-Fermi (DCF) method allows the characterization of the magnetized turbulence in molecular gas. The availability of high quality polarimetric data from instruments like HAWC+/SOFIA makes it possible to explore the spatial variations of the magnetic field structure and strength. In this talk, I will present an analysis that used the angular dispersion information to infer both the plane-of-sky (POS) and line-of-sight (LOS) components of the magnetic field in the Orion Molecular Cloud 1 (OMC-1) region. For the POS magnetic field, the angular dispersion analysis was performed within a moving kernel in order to construct maps of magnetized turbulence parameters and, in combination with auxiliary data, maps of the POS strength. For the LOS magnetic field, the relation between the local dispersion (i.e. RMS value) and the angle formed by the magnetic field with the LOS direction was explored, along with Zeeman measurements, as a mean to evaluate the strength of the LOS component. These maps of POS and LOS magnetic fields allow the calculation of the total magnetic field strength and therefore a map with more accurate values of the mass-to-magnetic flux (M/Phi). I will discuss the results of this analysis in the context of magnetic-field alignment with filamentary structures at different spatial scales.