  We present the spatially resolved gas and stellar kinematics of a sample of
ten hidden type 1 AGNs in order to investigate the true nature of the central
source and the scaling relation with host galaxy stellar velocity dispersion.
The sample is selected from a large number of hidden type 1 AGN, which are
identified based on the presence of a broad component in the \ha\ line profile
(i.e., full-width-at-half-maximum $>$ $\sim$1000 \kms), while they are often
mis-classified as type 2 AGN because AGN continuum and broad emission lines are
weak or obscured in the optical spectral range. We used the Blue Channel
Spectrograph at the 6.5-m MMT (Multiple Mirror Telescope) to obtain long-slit
data. We detected a broad \hb\ for only two targets, however, the presence of a
strong broad \ha\ indicates that these AGNs are low-luminosity type 1 AGNs. We
measured the velocity, velocity dispersion and flux of stellar continuum and
gas emission lines (i.e., \hb\ and \oiii) as a function of distance from the
center with a spatial scale of 0.3 arcsec pixel$^{-1}$. Spatially resolved gas
kinematics traced by \hb\ or \oiii\ are generally similar to stellar kinematics
except for the very center, where signatures of gas outflows are detected. We
compare the luminosity-weighted effective stellar velocity dispersion with
black hole mass, finding that these hidden type 1 AGN with relatively low back
hole mass follow the scaling relation of the reverberation-mapped type 1 AGN
and more massive inactive galaxies. }
