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In this paper we analyse the methodology to derive the bar pattern speed fromdynamical simulations. The results are robust to the changes in thevertical-scale height and in the mass-to-light (M/L) ratios. There is a smallrange of parameters for which the kinematics can be fitted. We have also takeninto account the use of different type of dynamical modelling and the effect ofusing 2-D vs 1-D models in deriving the pattern speeds. We conclude that thederivation of the bar streaming motions and strength and position of shocks isnot greatly affected by the fluid dynamical model used. We show new results onthe derivation of the pattern speed for NGC 1530. The best fit pattern speed isaround 10 km/s/kpc, which corresponds to a R_cor/R_bar = 1.4, implying a slowerbar than previously derived from more indirect assumptions. With this patternspeed, the global and most local kinematic features are beautifully reproduced.However, the simulations fail to reproduce the velocity gradients close to somebright HII regions in the bar. We have shown from the study of the Halphaequivalent widths that the HII regions that are located further away from thebar dust-lane in its leading side, downstream from the main bar dust-lane, areolder than the rest by 1.5-2.5 Myr. In addition, a clear spatial correlationwas found between the location of HII regions, dust spurs on the trailing sideof the bar dust-lane, and the loci of maximum velocity gradients parallel tothe bar major axis.

Deriving the pattern speed using dynamical modelling of gas flows in barred galaxies