Zappacosta, L., Piconcelli, E., Giustini, M., Vietri, G., Duras, F., Miniutti, G., Bischetti, M., Bongiorno, A., Brusa, M., Chiaberge, M., Comastri, A., Feruglio, C., Luminari, A., Marconi, A., Ricci, C., Vignali, C., Fiore, F. (2020). The WISSH quasars project VII. The impact of extreme radiative field in the accretion disc and X-ray corona interplay. Astronomy and Astrophysics 635, DOI: 10.1051/0004-6361/201937292
Hyper-luminous quasars (L-bol & x2004;greater than or similar to & x2004;10(47) erg s(-1)) are ideal laboratories to study the interaction and impact of the extreme radiative field and the most powerful winds in the active galactic nuclei (AGN) nuclear regions. They typically exhibit low coronal X-ray luminosity (L-X) compared to the ultraviolet (UV) and mid-infrared (MIR) radiative outputs (L-UV and L-UV); a non-negligible fraction of them report even similar to 1 dex weaker L-X compared to the prediction of the well established L-X-L-UV and L-X-L-UV relations followed by the bulk of the AGN population. In our WISE/SDSS-selected Hyper-luminous (WISSH) z & x2004;=& x2004;2 – 4 broad-line quasar sample, we report on the discovery of a dependence between the intrinsic 2-10 keV luminosity (L2 – 10) and the blueshifted velocity of the CIV emission line (v(CIV)) that is indicative of accretion disc winds. In particular, sources with the fastest winds (v(CIV) greater than or similar to 3000 km s(-1)) possess similar to 0.5-1 dex lower L2 – 10 than sources with negligible v(CIV). No similar dependence is found on L-UV, L-UV, L-bol, the photon index, or the absorption column density. We interpret these findings in the context of accretion disc wind models. Both magnetohydrodynamic and line-driven models can qualitatively explain the reported relations as a consequence of X-ray shielding from the inner wind regions. In case of line-driven winds, the launch of fast winds is favoured by a reduced X-ray emission, and we speculate that these winds may play a role in directly limiting the coronal hard X-ray production.