The Different Nature in Seyfert 2 Galaxies With and Without Hidden Broad-Line Regions

We compile a large sample of 120 Seyfert 2 galaxies (Sy2s) which contains 49 hidden broad-line region (HBLR) Sy2s and 71 non-HBLR Sy2s. From the difference in the power sources between two groups, we test if HBLR Sy2s are dominated by active galactic nuclei (AGNs), and if non-HBLR Sy2s are dominated by starbursts. We show that: (1) HBLR Sy2s have larger accretion rates than non-HBLR Sy2s; (2) HBLR Sy2s have larger \Nev $\lambda 14.32$/\Neii $\lambda 12.81$and\text{oiv}$\lambda 25.89$\mathrm{/}\text{Neii}$\lambda 12.81$ line ratios than non-HBLR Sy2s; (3) HBLR Sy2s have smaller $IRAS$ $f_{60}\mathrm{/}{f}_{25}$ flux ratio which shows the relative strength of the host galaxy and nuclear emission than non-HBLR Sy2s. So we suggest that HBLR Sy2s and non-HBLR Sy2s are AGN-dominated and starburst-dominated, respectively. In addition, non-HBLR Sy2s can be classified into the luminous ($L_{[\mathrm{O}\mathrm{I}\mathrm{I}\mathrm{I}]}>{10}^{41}\mathrm{e}\mathrm{r}\mathrm{g}\mathrm{s}{\mathrm{s}}^{-1}$) and less luminous ($L_{[\mathrm{O}\mathrm{I}\mathrm{I}\mathrm{I}]}<{10}^{41}\mathrm{e}\mathrm{r}\mathrm{g}\mathrm{s}{\mathrm{s}}^{-1}$) samples, when considering only their obscuration. We suggest that: (1) the invisibility of polarized broad lines (PBLs) in the luminous non-HBLR Sy2s depends on the obscuration; (2) the invisibility of PBLs in the less luminous non-HBLR Sy2s depends on the very low Eddington ratio rather than the obscuration.