a demarcation line, the northern section shows an organized “$\overrightarrow{B}$-vectors” V-pattern along the outflows in the 230 GHz CARMA dataset. As it gets closer to the central region, with an increase in resolution and change of wavelength (870 $\mu$m SMA and ALMA dataset), we observe a remarkable consistency in the general distribution of the vectors. This would suggest that the mechanism responsible for aligning the dust grains, that we assume to be the magnetic field, is strong and coherent enough (the vectors showing a noticeable organized pattern) that it is not disturbed along most of the extent of the northern lobe.\
Another significant point is that from the global “V-shaped” structure observed with CARMA (Fig.\[CompB\]-left), a complete hourglass becomes even clearer down to the ALMA resolution. Indeed, the set of $\overrightarrow{B}$-vectors in the region noted “D” in the SMA observations at PA=-20 (Fig.\[CompB\]-middle) and the ones in the region noted “B2” in the ALMA observations at PA= -18 (Fig.\[CompB\]-right) seems to draw the southern section of the magnetic hourglass. In all the maps, the center of this bipolar pattern appears to be coincident with the approximate location of the central star.\
While the Stokes I flux densities of both the 