Binned results of the normalised SFR as a function of the median AGN X-ray luminosity, in bins of normalized SFR. Left panel: filled circles present the measurements for the 3336 sources. Open squares show our estimates when we restrict our sample to those X-ray AGN with log L_X(2 − 10 keV) > 43.5 erg s⁻¹ to account for the L_X-z incompleteness of our dataset (see Fig. 2 and text for more details). Right panel: our results for the 608/3336 AGN with available Herschel photometry (filled squares). Open squares show our measurements for the 381 sources with Herschel photometry and log L_X(2 − 10 keV) > 43.5 erg s⁻¹. In both panels the dashed line corresponds to AGN in the main sequence. Above this line, AGN have an enhanced SFR compared to star formation main-sequence galaxies of the same stellar mass and redshift. Below the dashed line, AGN have an SFR that is suppressed compared to main-sequence galaxies of the same mass and redshift. Based on our results, the AGN enhances the star formation of its host galaxy when the latter lies below the main sequence (below the dashed line) and quenches the star formation of the galaxy it lives in when the host lies above the main sequence (above the dashed line).