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We present a study of optically-selected Type II AGN at 0.5 < z < 0.9 fromthe VIPERS and VVDS surveys, to investigate the connection between AGN activityand physical properties of their host galaxies. The host stellar mass isestimated through spectral energy distribution fitting with the CIGALE code,and star formation rates are derived from the [OII]$\lambda$3727 $\r{A}$ lineluminosity. We find that 49% of the AGN host galaxies are on or above the mainsequence (MS), 40% lie in the sub-MS locus, and 11% in the quiescent locus.Using the [OIII]$\lambda$5007 $\r{A}$ line luminosity as a proxy of the AGNpower, we find that at fixed AGN power Type II AGN host galaxies show a bimodalbehaviour: systems with host galaxy stellar mass <10$^{10}$ M$_{\odot}$, residealong the MS or in the starbursts locus (high-SF Type II AGN), while systemsresiding in massive host-galaxies (>10$^{10}$ M$_{\odot}$) show a lower levelof star formation (low-SF Type II AGN). At all stellar masses, the offset fromthe MS is positively correlated with the AGN power. We interpret thiscorrelation as evidence of co-evolution between the AGN and the host, possiblydue to the availability of cold gas. In the most powerful AGN with hostgalaxies below the MS we find a hint, though weak, of asymmetry in the [OIII]line profile, likely due to outflowing gas, consistent with a scenario in whichAGN feedback removes the available gas and halts the star formation in the mostmassive hosts.

The Type II AGN-host galaxy connection: insights from the VVDS and VIPERS surveys