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We acquired spectra of 141 HII regions in ten late-type low surfacebrightness galaxies (LSBGs). The analysis of the chemical abundances obtainedfrom the nebular emission lines shows that metallicity gradients are a commonfeature of LSBGs, contrary to previous claims concerning the absence of suchgradients in this class of galaxies. The average slope, when expressed in unitsof the isophotal radius, is found to be significantly shallower in comparisonto galaxies of high surface brightness. This result can be attributed to thereduced surface brightness range measured across their discs, when combinedwith a universal surface mass density-metallicity relation. With a similarargument we explain the common abundance gradient observed in high surfacebrightness galaxy (HSBG) discs and its approximate dispersion. This conclusionis reinforced by our result that LSBGs share the same common abundance gradientwith HSBGs, when the slope is expressed in terms of the exponential disc scalelength.

Abundance gradients in low surface brightness spirals: clues on the origin of common gradients in galactic discs