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We aim to understand what drives the IRX-\beta dust attenuation relation atintermediate redshift (0.5 < z < 0.8) in star-forming galaxies. We investigatethe role of various galaxy properties in shaping this observed relation. We userobust [O ii] {\lambda}3727, [O iii] {\lambda}{\lambda}4959, 5007, and H\betaline detections of our statistical sample of 1049 galaxies to estimate thegas-phase metallicities. We derive key physical properties that are necessaryto study galaxy evolution, such as the stellar masses and the star formationrates, using the spectral energy distribution fitting tool CIGALE.Equivalently, we study the effect of galaxy morphology (mainly the S\'ersicindex n and galaxy inclination) on the observed IRX-\beta scatter. We alsoinvestigate the role of the environment in shaping dust attenuation in oursample. We find a strong correlation of the IRX-\beta relation on gas-phasemetallicity in our sample, and also strong correlation with galaxy compactnesscharacterized by the S\'ersic indexes. Correlations are also seen with stellarmasses, specific star formation rates and the stellar ages of our sources.Metallicity strongly correlates with the IRX-\beta scatter, this also resultsfrom the older stars and higher masses at higher beta values. Galaxies withhigher metallicities show higher IRX and higher beta values. The correlationwith specific dust mass strongly shifts the galaxies away from the IRX-\betarelation towards lower \b{eta} values. We find that more compact galaxieswitness a larger amount of attenuation than less compact galaxies. There is asubtle variation in the dust attenuation scatter between edge-on and face-ongalaxies, but the difference is not statistically significant. Galaxyenvironments do not significantly affect dust attenuation in our sample ofstar-forming galaxies at intermediate redshift.

Decoding the IRX-\beta\ dust attenuation relation in star-forming galaxies at intermediate redshift