Figure 6: The separation between Seyfert 2 with detection of polarized broad lines (hidden BLR, HBLR) and Seyfert 2s without polarized broad lines (non-HBLR) is clear both in X-ray luminosity and Eddington rate, when only Compton-thin sources are taken into account. However, a number of Compton-thick Non-HBLR sources have high accretion rates and luminosity, suggesting that obscuration also plays an important role in the detection of the HBLR (from Marinucci et al. [113]).