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Gas inflowing along stellar bars is often stalled at the location ofcircumnuclear rings, that form an effective reservoir for massive starformation and thus shape the central regions of galaxies. However, how exactlystar formation is proceeding within these circumnuclear starburst rings issubject of debate. Two main scenarios for this process have been put forward:In the first the onset of star formation is regulated by the total amount ofgas present in the ring with star forming starting once a mass threshold hasreached in a `random' position within the ring like `popcorn'. In the secondstar formation preferentially takes place near the locations where the gasenters the ring. This scenario has been dubbed `pearls-on-a-string'. Here wecombine new optical IFU data covering the full stellar bar with existingmulti-wavelength data to study in detail the 580 pc radius circumnuclearstarburst ring in the nearby spiral galaxy NGC 6951. Using HST archival datatogether with Sauron and Oasis IFU data, we derive the ages and stellar massesof star clusters as well as the total stellar content of the central region.Adding information on the molecular gas distribution, stellar and gaseousdynamics and extinction, we find that the circumnuclear ring in NGC 6951 is~1-1.5 Gyr old and has been forming stars for most of that time. We seeevidence for preferred sites of star formation within the ring, consistent withthe `pearls-on-a-string' scenario, when focusing on the youngest stellarpopulations. Due to the ring's longevity this signature is washed out whenolder stellar populations are included in the analysis.

How does star formation proceed in the circumnuclear starburst ring of NGC 6951?