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Star formation (SF) takes place in unusual places such as way out in theintergalactic medium out of material expelled from parent galaxies. We wish toanswer whether SF proceeds in this specific environment in a similar way thanin galactic disks. We have carried out a multiwavelength analysis of theinteracting system NGC 5291, which is remarkable for its extended HI ringhosting numerous intergalactic HII regions. We combined new ultraviolet (GALEX)observations with archival Halpha, 8 mu m (Spitzer Space Telescope) and HI (VLAB-array) images of the system. We have found that the morphology of the starforming regions, as traced by the ultraviolet, Halpha, and 8 mu m emission issimilar. There is a clear excess of ultraviolet emission compared to individualHII regions in spirals, i.e. the [8.0]/[NUV] and [Halpha]/[NUV] SFR ratios areon average low although there are some large variations from one region toanother, which cannot be explained by variations of the metallicity or the dustextinction along the HI structure. Comparing the observed SFR with a model ofthe evolution of [Halpha]/[NUV] with time favours young, quasi-instantaneousthough already fading starbursts. The total star formation rate measured in theintergalactic medium (which accounts for 80% of the total) surrounding NGC 5291is up to 1.3 Msun/yr, a value typical for spirals, assuming the standard SFRcalibrations are valid. The SFR drops by a factor of 2 to 4 in case the starformation is indeed quasi-instantaneous. (abridged)

Polychromatic view of intergalactic star formation in NGC 5291