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

Larger $\lambda_R$ in the disc of isolated active spiral galaxies than in their non-active twins