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We present emission line mapping of the strongly barred galaxy NGC 1530obtained from Fabry-Perot interferometry in Halpha, at significantly enhancedangular resolution compared with published studies. The main point of the workis to examine in detail the non-circular components of the velocity field ofthe gas, presumably induced by the strongly non-axisymmetric gravitationalpotential of the bar. These reveal quasi-elliptical motions with speeds oforder 100 km/s aligned with the bar. It also shows how these flows swing intowards and around the nucleus as they cross a circumnuclear resonance, fromthe dominant "x1 orbits" outside the resonance to "x2 orbits" within it.Comparing cross-sections of the residual velocity map along and across the barwith the Halpha intensity map indicates a systematic offset between regions ofhigh non-circular velocity and massive star formation. To investigate furtherwe produce velocity gradient maps along and across the bar. These illustratevery nicely the shear compression of the gas, revealed by the location of thedust lanes along loci of maximum velocity gradient perpendicular to the bar.They also show clearly how shear acts to inhibit massive star formation,whereas shocks act to enhance it. Although the inhibiting effect of gas shearflow on star formation has long been predicted, this is the clearestobservational illustration so far of the effect. It is also the clearestevidence that dust picks out shock-induced inflow along bars. Theseobservations should be of considerable interest to those modelling massive starformation in general.

Ionized gas kinematics and massive star formation in NGC 1530