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The ultraviolet (UV) upturn is characterised by an unexpected up-rise of theUV flux in quiescent galaxies between the Lyman limit and 2500\AA. By makinguse of colour-colour diagrams, one can subdivide UV bright red-sequencegalaxies in two groups: UV weak and upturn. With these two groups, we propose acomparison between their stellar population properties with the goal ofestablishing differences and similarities between them. We make use ofpropensity score matching (PSM) to mitigate potential biases between the twosamples, by selecting similar objects in terms of redshift and stellar mass.Also, we take advantage of spectral energy distribution (SED) fitting resultsfrom magphys made available by the GAMA collaboration. The analyses are made bycomparing the distributions from the SED fitting directly, as well asinvestigating the differences in correlations between their parameters, andfinally by using principal component analysis (PCA). We explore importantdifferences and similarities between UV weak and upturn galaxies in terms ofseveral parameters, such as: metallicity, age, specific star formation rate,time of last burst of star-formation, to mention a few. Notable differences arethose concerning (g-r) colour, metallicity, and time since last burst ofstar-formation: UV upturn are redder in the optical, more metallic, and theirlast burst of star-formation happened earlier in time. These differencessuggest that UV upturn systems have shorter star-formation histories (i.e. havebeen evolving more passively) when compared to UV weak galaxies. Consequently,these last seem to have a higher diversity of stellar populations.

UV upturn versus UV weak galaxies: differences and similarities of their stellar populations unveiled by a de-biased sample