flux of 23$\pm$3 mJy beam$^{-1}$ and a peak of 46$\pm$5 mJy beam$^{-1}$.\
The polarization map, shown in Fig.\[Evectors\], indicates the global distribution of the electric vectors ($\overrightarrow{E}$-vectors) and we emphasize that the dusty regions in the nebula where those vectors are not indicated have a polarized intensity below 3$\sigma$. The polarized emission is not uniform but is rather patchy with three main regions (noted A, B and C in Fig.\[Evectors\]). The peak polarization (P$_{\it{Pol}}$), located at the coordinates 07$^{h}$42$^{m}$16$^{s}$976 -14$\degr$42$\arcmin$49$\farcs$357 inside the area B, has a measured flux of 1.13$\pm$0.3 mJy beam$^{-1}$. As observed in many astronomical objects, including OH 231.8+4.2 (see @Sabin2014 [@Sabin2015b]), P$_{\it{Pol}}$ and P$_{\it{Int}}$ are not spatially coincident.\
Most of the $\overrightarrow{E}$-vectors are relatively well organized within each area and this is particularly seen in regions A and B. We found mean position angles for the electric vectors (EVPA) of about -19$\pm$2 and -42$\pm$3 for the regions A and B respectively. However, while the mean PA seems to indicate a global preferential alignment direction of the dust grains in these two regions, locally we observe a curvature in the distribution of the position angle of the $\overrightarrow{E}$-vectors, which is likely to be of interest for the understanding 