\begin{table}%t1
\caption{The properties for 12 type II AGNs with HBLRs.}\label{tab1}
\small
%\centerline
{
\begin{tabular}{lcccccccc}\hline \hline
name & z & log~($L_{\rm [O~III]}$)&${\it FWHM}_{\rm [O~III]}$&$\sigma_{\ast}$& ${\it FWHM}_{\hb}$&log~($M_{\hb}/\msun$)&log~($M_{\sigma_*}/\msun$)& Ref.\\
     &   &  $\ergs$  &        $\kms$            & $\kms$      & $\kms$         &                     &                   &\\
(1) & (2) &(3) & (4) & (5) & (6) & (7) & (8)& (9)\\
 \hline
NGC1068 & 0.004 & 42.645$^a$ & --  & 128 & 3030 & 7.88 & 7.35 & $1,1,2$\\
NGC7212 & 0.027 & 42.636$^a$ & --  & 137 & 5420 & 8.37 & 7.47 & $1,1,2$\\
NGC7674 & 0.029 & 42.495$^a$ & --  & 144 & 2830 & 7.82 & 7.56 & $1,1,2$\\
Mrk3    & 0.014 & 43.221$^a$ & --  & 269 & 6000 & 9.17 & 8.65 & $1,1,2$\\
Mrk348  & 0.015 & 41.912$^a$ & --  & 185 & 9350 & 8.17 & 7.99 & $1,1,2$\\
Mrk463E & 0.050 & 42.785$^a$ & --  & 137 & 2770 & 7.81 & 7.88 & $1,1,2$\\
Mrk477  & 0.038 & 43.543$^a$ & --  & 117 & 4130 & 8.84 & 7.19 & $1,1,2$\\
Mrk1210 & 0.013 & 42.195$^a$ & --  & 77  & 3080 & 7.90 & 6.46 & $1,1,2$\\
J0842+3625 & 0.561 & 43.601$^b$ & 303.76 &129.30$^c$ & 4900($H_{\gamma}$) &8.99 &7.37 & $3,3,4$\\
J1039+6430 & 0.402 & 42.901$^b$ & 385.75 &164.15$^c$ & 3070 & 7.89 & 7.79 & $3,3,4$ \\
J1543+4935 & 0.512 & 42.789$^b$ & 709.72 &302.01$^c$ & 4300 & 8.19 &8.84 & $3,3,4$\\
J1641+3858 & 0.596 & 43.474$^b$ & 395.72 &168.39$^c$ & 3200($H_{\gamma}$) & 8.62 &7.83 &$3,3,4$\\
\hline
\end{tabular}}
\medskip
 Notes. -- Col. (1),
name; Col. (2), redshift; Col.~3, the \oiii\ luminosity; Col. (4),
{\it FWHM} of the narrow \oiii\ line; Col. (5), stellar velocity
dispersion; Col. (6), {\it FWHM} of H$\beta$ from HBLRs; Col. (7), SMBH
masses derived from the polarimetric broad line; Col. (8), SMBH
masses derived from the $\mbh - \sigma_*$ relation. Col. (9),
reference for Cols. (3,5,6): (1) Bian \& Gu (\cite{Bian2007}); (2) Tran (\cite{Tran1995}); (3)
this work; (4) Zakamska et~al. (\cite{Zakamska2005}). $^a$: the intrinsic
extinction-corrected \oiii\ luminosity; $^b$: the intrinsic
extinction-uncorrected \oiii\ luminosity; $^c$: the stellar velocity
dispersion is derived from the {\it FWHM} of the narrow/core \oiii.
\end{table}