The first 62 AGN observed with SDSS-IV MaNGA -- III: stellar and gas
  kinematics
  We investigate the effects of Active Galactic Nuclei (AGN) on the gas
kinematics of their host galaxies, using MaNGA data for a sample of 62 AGN
hosts and 109 control galaxies (inactive galaxies). We compare orientation of
the line of nodes (kinematic Position Angle - PA) measured from the gas and
stellar velocity fields for the two samples. We found that AGN hosts and
control galaxies display similar kinematic PA offsets between gas and stars.
However, we note that AGN have larger fractional velocity dispersion $\sigma$
differences between gas and stars [$\sigma_{frac}=(\sigma_{\rm
gas}-\sigma_{stars})/\sigma_{\rm stars}$] when compared to their controls, as
obtained from the velocity dispersion values of the central (nuclear) pixel
(2.5" diameter). The AGN have a median value of $\sigma_{\rm frac}$ of
$<\sigma_{frac}>_{\rm AGN}=0.04$, while the the median value for the control
galaxies is $<\sigma_{frac}>_{\rm CTR}=-0.23$. 75% of the AGN show
$\sigma_{frac}>-0.13$, while 75% of the normal galaxies show $\sigma_{\rm
frac}<-0.04$, thus we suggest that the parameter $\sigma_{\rm frac}$ can be
used as an indicative of AGN activity. We find a correlation between the
[OIII]$\lambda$5007 luminosity and $\sigma_{frac}$ for our sample. Our main
conclusion is that the AGN already observed with MaNGA are not powerful enough
to produce important outflows at galactic scales, but at 1-2 kpc scales, AGN
feedback signatures are always present on their host galaxies.
