Are there larger stellar velocity dispersions in low redshift Type-1 AGN
  than in Type-2 AGN?
  The main objective is to check the Unified Model (UM) expected similar
stellar velocity dispersions between Type-1 AGN and Type-2 AGN, then to provide
further clues on BH mass properties. Not similar as previous comparisons of BH
masses estimated by \msig relations to Type-2 AGN but Virial BH masses in
Type-1 AGN, reliable stellar velocity dispersions $\sigma$ measured through
absorption features around 4000\AA~ are directly compared between so-far the
largest samples of 6260 low redshift ($z~<~0.3$) Type-1 AGN and almost all the
Type-2 AGN in SDSS DR12. Although half of Type-1 AGN do not have measured
$\sigma$ due to unapparent absorption features overwhelmed by AGN activities,
both properties of mean spectra of Type-1 AGN with and without measured
$\sigma$ and positive dependence of $\sigma$ on [O~{\sc iii}] luminosity can
lead to statistically larger $\sigma$ of all the Type-1 AGN than the 6260
Type-1 AGN with measured stellar velocity dispersions. Then, direct $\sigma$
comparisons can lead to statistically larger $\sigma$ in Type-1 AGN, with
confidence level higher than 10sigma, after considering necessary effects of
different redshift and different central AGN activities. Although Type-1 AGN
have $\sigma$ only about $(9\pm3)$\% larger than Type-2 AGN, the difference
cannot be well explained at current stage. Unless there was strong evidence to
support different \msig relations or to support quite different evolution
histories between Type-1 AGN and Type-2 AGN, the statistically larger $\sigma$
in Type-1 AGN provides a strong challenge to the Unified model of AGN.
