Larger $\lambda_R$ in the disc of isolated active spiral galaxies than
  in their non-active twins
  We present a comparison of the spin parameter $\lambda_R$, measured in a
region dominated by the galaxy disc, between 20 pairs of nearby
(0.005$<$z$<$0.03) seemingly isolated twin galaxies differing in nuclear
activity. We find that 80--82% of the active galaxies show higher values of
$\lambda_R$ than their corresponding non-active twin(s), indicating larger
rotational support in the AGN discs. This result is driven by the 11 pairs of
unbarred galaxies, for which 100% of the AGN show larger $\lambda_R$ than their
twins. These results can be explained by a more efficient angular momentum
transfer from the inflowing gas to the disc baryonic matter in the case of the
active galaxies. This gas inflow could have been induced by disc or bar
instabilities, although we cannot rule out minor mergers if these are prevalent
in our active galaxies. This result represents the first evidence of
galaxy-scale differences between the dynamics of active and non-active isolated
spiral galaxies of intermediate stellar masses (10$^{10}<M_*<10^{11}$
M$_{\odot}$) in the Local Universe.
