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We investigate the effects of Active Galactic Nuclei (AGN) on the gaskinematics of their host galaxies, using MaNGA data for a sample of 62 AGNhosts and 109 control galaxies (inactive galaxies). We compare orientation ofthe line of nodes (kinematic Position Angle - PA) measured from the gas andstellar velocity fields for the two samples. We found that AGN hosts andcontrol 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 [$\sigma_{frac}=(\sigma_{\rmgas}-\sigma_{stars})/\sigma_{\rm stars}$] when compared to their controls, asobtained 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 controlgalaxies is $<\sigma_{frac}>_{\rm CTR}=-0.23$. 75% of the AGN show$\sigma_{frac}>-0.13$, while 75% of the normal galaxies show $\sigma_{\rmfrac}<-0.04$, thus we suggest that the parameter $\sigma_{\rm frac}$ can beused as an indicative of AGN activity. We find a correlation between the[OIII]$\lambda$5007 luminosity and $\sigma_{frac}$ for our sample. Our mainconclusion is that the AGN already observed with MaNGA are not powerful enoughto produce important outflows at galactic scales, but at 1-2 kpc scales, AGNfeedback signatures are always present on their host galaxies.

The first 62 AGN observed with SDSS-IV MaNGA -- III: stellar and gas kinematics