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You can acquire the latest and greatest in ESET Remote Administrator by upgrading your license key and downloading the. called L, most importantly the polarized six lines around H$\alpha$ and H$\beta$ that are due to a combination of and the Zeeman effect. A careful analysis of this spectral region has been performed in the last years by a number of authors, mainly by @bd17 [@bd20] and @bel20 [@bel21] who found the large majority of the targets, except maybe a few, to be type B Seyferts. The presence of a hidden region explains the emission in forbidden lines in at least some AGN. This picture is in line with other recent spectropolarimetric studies [@sai20; @sai21; @bel16; @bel17] that, using polarization spectra, estimated the fraction of type B Seyferts to be above 80%. This conclusion is confirmed in Fig. \[bvsn\] where we compare the B/N ratio of and type B Seyfert galaxies. The discovery of polarized emission in all of the selected AGN, but in few cases from a small fraction of objects, is very rare, if not unprecedented. In order to show that this effect is not due to any single object we are able to derive the intrinsic polarization of our targets using the peak polarization value (Ppeak). The original polarization spectra were stored in the catalog and then analyzed by a routine in [*poldy*]{} (Kudryavtsev et al. in prep.). We selected for our analysis the red part of the polarization spectra, where the maximum polarization, due to its intrinsic wavelength dependence, can be derived by fitting gaussians to the line profiles. We did not include the blue part of the spectra, where the emission is due to the superposition of atomic and molecular lines whose polarized emission is very low. Using this method we derived the average polarization, Pave, of our selected targets. From the plot, we are able to show that the stars are unpolarized within the statistical errors, confirming that the polarization seen in the AGN is real. Note that the method presented in this paper was not able to detect any high redshift object. Our sample is actually constituted by objects in the range $0.02<z<0.75$ while the higher

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