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Within the NUclei of GAlaxies project we have obtained IRAM PdBI and 30m12CO(1-0) and 12CO(2-1) observations of the spiral galaxy NGC 6951. Previouswork shows that there is indirect evidence of gas inflow from 3 kpc down tosmall radii: a large-scale stellar bar, a prominent starburst ring (r~580 pc)and a LINER/Seyfert 2 nucleus. In this paper we study the gas kinematics astraced by the CO line emission in detail. We quantify the influence of thelarge-scale stellar bar by constructing an analytical model of the evolution ofgas particles in a barred potential. From this model gravitational torques andmass accumulation rates are computed. We compare our model-based gravitationaltorque results with previous observationally-based ones. The model also showsthat the large-scale stellar bar is indeed the dominant force for driving thegas inward, to the starburst ring. Inside the ring itself a nuclear stellaroval might play an important role. Detailed analysis of the CO gas kinematicsthere shows that emission arises from two co-spatial, but kinematicallydistinct components at several locations. The main emission component canalways be related to the overall bar-driven gas kinematics. The secondcomponent exhibits velocities that are larger than expected for gas on stableorbits, has a molecular gas mass of 1.8x10^6Msun, is very likely connected tothe nuclear stellar oval, and is consistent with inflowing motion towards thevery center. This may form the last link in the chain of gas inflow towards theactive galactic nucleus in NGC 6951.

Molecular gas in NUclei of GAlaxies (NUGA) XV. Molecular gas kinematics in the inner 3kpc of NGC6951