  We analyse the kinematics of 170 AGN host galaxies as compared to those of a
matched control sample of non-active galaxies from the MaNGA survey in order to
characterise and estimate the extents of the Narrow Line Region (NLR) and of
the kinematically disturbed region (KDR) by the AGN. We define the observed NLR
radius as the farthest distance from the nucleus within which both
[Oiii]/H\beta and [Nii]/H\alpha ratios fall in the AGN region of the BPT
diagram and the H\alpha equivalent width is required to be larger than 3.0\AA.
The extent of the KDR is defined as the distance from the nucleus within which
the AGN hosts galaxies shows a more disturbed gas kinematics than the control
galaxies. The kinematics derived from the [Oiii] line profiles reveal that, on
average, the most luminous AGN (L[Oiii] > 3.8 * 10^40 erg s^-1) possess higher
residual difference between the gaseous and stellar velocities and velocities
dispersion than their control galaxies. Spatially resolved NLR's and KDR's were
found in 55 and 46 AGN host galaxies, with corrected radii 0.2 < r_KDR,c < 2.3
kpc and 0.4 < r_NLR,c < 10.1 kpc, with a relation between the two given by log
r_KDR,c = (0.53\pm0.12) log r_NLR,c + (1.07\pm0.22), respectively. The
extension of the KDR corresponds to about 30 per cent of that of the NLR.
Assuming that the KDR is due to an AGN outflow, we have estimated ionised gas
mass outflow rates that range between 10^-5 and \approx 1 Myr^-1, and kinetic
powers that range from 10^34 to 10^40 erg s^-1. Comparing the power of the AGN
ionised outflows with the AGN luminosities, they are always below the 0.05
L_AGN model threshold for having an important feedback effect on their
respective host galaxies. The mass outflow rates (and power) of our AGN sample
correlate with their luminosities, populating the lowest AGN luminosity range
of the correlations previously found for more powerful sources.
