The relevance of the Tremaine-Weinberg ( TW ) method is tested to measure the bar , spiral and inner structure pattern speeds using a gaseous velocity field .
The TW method is applied to various simulated barred galaxies in order to demonstrate its validity in seven different configurations , including star formation or/and dark matter halo .
The reliability of the different physical processes involved and of the various observational parameters are also tested .
The simulations show that the TW method could be applied to the gaseous velocity fields to get a good estimate of the bar pattern speed , under the condition that regions of shocks are avoided and measurements are confined to regions where the gaseous bar is well formed .
We successfully apply the TW method to the H \alpha velocity field of the Virgo Cluster Galaxy M100 ( NGC 4321 ) and derive pattern speeds of 55 \pm 5 km s ^ { -1 } kpc ^ { -1 } for the nuclear structure , 30 \pm 2 km s ^ { -1 } kpc ^ { -1 } for the bar and 20 \pm 1 km s ^ { -1 } kpc ^ { -1 } for the spiral pattern , in full agreement with published determinations using the same method or alternative ones .