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Large future sky surveys, such as the LSST, will provide optical photometryfor billions of objects. This paper aims to construct a proxy for the farultraviolet attenuation (AFUVp) from the optical data alone, enabling the rapidestimation of the star formation rate (SFR) for galaxies that lack UV or IRdata. To mimic LSST observations, we use the deep panchromatic optical coverageof the SDSS Photometric Catalogue DR~12, complemented by the estimated physicalproperties for the SDSS galaxies from the GALEX-SDSS-WISE Legacy Catalog(GSWLC) and inclination information obtained from the SDSS DR7. We restrictedour sample to the 0.025-0.1 z-spec range and investigated relations amongsurface brightness, colours, and dust attenuation in the far UV range forstar-forming galaxies obtained from the spectral energy distribution (SED).{Dust attenuation is best correlated with (u-r) colour and the surfacebrightness in the u band ($\rm \mu_{u}$). We provide a dust attenuation proxyfor galaxies on the star-forming main sequence, which can be used for the LSSTor any other type of broadband optical survey. The mean ratio between thecatalogue values of SFR and those estimated using optical-only SDSS data withthe AFUVp prior calculated as $\Delta$SFR=log(SFR$_{\tiny{\mbox{thiswork}}}$/SFR$_{\tiny{}\texttt{GSWLC}}$) is found to be less than 0.1~dex, whileruns without priors result in an SFR overestimation larger than 0.3~dex. Thepresence or absence of theAFUVp has a negligible influence on the stellar massestimation (with $\Delta$M$_{star}$ in the range from 0 to $-0.15$ dex).Forthcoming deep optical observations of the LSST Deep Drilling Fields, whichalso have multi-wavelength data, will enable one to calibrate the obtainedrelation for higher redshift galaxies and, possibly, extend the study towardsother types of galaxies, such as early-type galaxies off the main sequence.

Attenuation proxy hidden in surface brightness-colour diagrams. A new strategy for the LSST era