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NGC 2903 is a nearby barred spiral with an active starburst in the center andHii regions distributed along its bar. We aim to analyse the star formationproperties in the bar region of NGC 2903 and study the links with the typicalbar morphological features. A combination of space and ground-based data fromthe far-ultraviolet to the sub-millimeter spectral ranges is used to create apanchromatic view of the NGC 2903 bar. We produce two catalogues: one for thecurrent star formation regions, as traced by the halpha compact emission, and asecond one for the ultraviolet (UV) emitting knots, containing positions andluminosities. From them we have obtained ultraviolet colours, star formationrates, dust attenuation and halpha EWs, and their spatial distribution havebeen analysed. Stellar cluster ages have been estimated using stellarpopulation synthesis models (Starburst99). NGC 2903 is a complex galaxy, with avery different morphology on each spectral band. The CO(J=1-0) and the 3.6micron emission trace each other in a clear barred structure, while the halphaleads both components and it has an s-shape distribution. The UV emission ispatchy and does not resemble a bar. The UV emission is also characterised by anumber of regions located symmetrically with respect to the galaxy center,almost perpendicular to the bar, in a spiral shape covering the inner ~2.5 kpc.These regions do not show a significant halpha nor 24 micron emission. We haveestimated ages for these regions ranging from 150 to 320 Myr, being older thanthe rest of the UV knots, which have ages lower than 10 Myr. The SFR calculatedfrom the UV emission is ~0.4 M$_{\odot}$/yr, compatible with the SFR as derivedfrom halpha calibrations (M$_{\odot}$/yr).

Multiwavelength study of the star formation in the bar of NGC 2903