We present observations of the barred spiral galaxy NGC 1530 that we use to investigate the overall structure and gas content of the galaxy. We use sensitive Hα Fabry-Perot observations of the ionized gas to determine the star forming rates in various regions of the galaxy. Westerbork H I observations are used to investigate the morphology of the atomic gas and combined with the Hα Fabry-Perot to determine the rotation curve. From the rotation curve we derive a pattern speed of the bar of approximately 20 km s^-1^ kpc^-1^ that predicts resonances at locations that coincide with prominent morphological features, including three gaseous rings mapped in these observations: an outer ring of atomic hydrogen at a radius consistent with the outer Lindblad resonance, an inner ring seen in both atomic hydrogen and Hα, and a nuclear ring of dust and molecular gas. These rings combined with the very strong spiral arms dominate the morphology of the galaxy.