spots located at opposite sides of the star indicated a strength of the magnetic field along the line of sight of 44$\pm$7 mG and -29$\pm$21 mG. The extrapolation of the field’s strength to the stellar surface, assuming a toroidal distribution, sets a value of $\sim$2.5 G at 1 R$\star$.\
Finally, @Sabin2014 [@Sabin2015b] mapped the polarized thermal emission of the dust continuum at submillimeter (0.87mm/345 GHz) and millimeter (1.3mm/230 GHz) range with the Submillimeter Array (SMA) and Combined Array for Research in Millimeter-wave Astronomy (CARMA), respectively. Based on the radiative torques (RATs) theory regarding the alignment of non-spherical spinning dust grains with respect to the magnetic field [@Lazarian2007; @Lazarian2008; @Hoang2008; @Lazarian2011], the authors were able to infer the presence of an X-shaped magnetic field distribution centred at the base of each optical outflow and encompassing the red- and blue-shifted $^{12}$CO ([*J*]{}=3$\rightarrow$2) molecular outflows. The 230 GHz polarimetric analysis also indicates an organized magnetic field, which not only mirrors part of the X-shaped structure seen at the submillimeter wavelength, but most importantly it also shows the presence of a new structure aligned with the equatorial plane of the nebula. The combined analysis thus revealed the coexistence of an inner dipole/polar magnetic field 