Comparison of the best-fit solution SED modelling parameters (from top to bottom : T_*, T_inn, n and τ₅₅₀) with P (left) and $R_{\mathrm{F}\mathrm{U}\mathrm{V}/\mathrm{N}\mathrm{U}\mathrm{V}}^{\mathrm{c}\mathrm{o}\mathrm{r}\mathrm{r}}$ (right). The colour and shape of the markers represent the stellar variability and chemistry type as in Fig. 4. The horizontal line in the third row represents n=2. Error bars of $R_{\mathrm{F}\mathrm{U}\mathrm{V}/\mathrm{N}\mathrm{U}\mathrm{V}}^{\mathrm{c}\mathrm{o}\mathrm{r}\mathrm{r}}$ include the multi-epoch variability of sources detected in both GALEX bands, arrows indicate that one observation was an upper limit.