at most only over a semi-major axis of $\sim$7. This represents $\sim$2.6 times less than the optical northern lobe and 5.1 times less than the southern one. The thermal dust emission observed with our combined dataset, therefore traces the highest dust density regions of the nebula (see also @Balick2017 and @SC2018). Fig.\[CompB\] presents three distinct behaviours (or distributions) of the magnetic fields in the regions above and below the equatorial plane. They are described in the following sections \[reg1\], \[reg2\] and \[reg3\].

Poloidal or hourglass magnetic distribution {#reg1}
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The analysis of the ALMA polarization data shows that the $\overrightarrow{B}$-vectors (EVPA rotated by 90) located in the areas A (with a mean PA=63), B1 (with a mean PA=23) and B3 (with mean a PA=-25) align quite well with the edges of the northern outflow within its opening angle of 67 (with a mean PA= 23 based on the optical HST image presented here). The uncertainty on the polarization angles, assuming a 3$\sigma$ threshold, was estimated to be around 10% using the relation derived by @Serkowski74. We can now integrate all the information to assess the distribution of the magnetic field. With the equator of the nebula (at PA $\sim$113) as 