摘要：We performed a survey of the X-ray properties of 41 objects from the WISE/SDSS selected hyper-luminous (WISSH) quasars sample, which includes 86 broad-line quasars with bolometric luminosityLBol≳ 2 × 1047erg s-1shining atz~ 2–4. We used both proprietary and archivalChandraandXMM-Newtonobservations. Twenty-one quasars have sufficient quality data to perform a spectroscopic analysis, while for the remaining sources, X-ray properties are derived through hardness-ratio analysis (apart for six sources that result to be undetected). The bulk (~70%) of the detected WISSH quasars exhibitNH<5 × 1022cm-2, in agreement with their optical Type 1 AGN classification. All but three quasars show unabsorbed 2–10 keV luminositiesL2−10≥1045erg s-1. Thanks to their extreme radiative output across the mid-IR-to-X-ray range, WISSH quasars therefore offer the opportunity to significantly extend and validate the existing relations involvingL2−10. Specifically, we studied the X-ray luminosity as a function of (i) X-ray-to-optical (X/O) flux ratio; (ii) mid-IR luminosity (LMIR); (iii)LBol, and (iv)αOXversus 2500 Å luminosity. We find that the WISSH quasars show (i) unreported very low X/O (<0.1) compared to typical AGN values; (ii)L2−10/LMIRratios that are significantly smaller than those derived for AGN with lower luminosity; (iii) a large X-ray bolometric correction,kBol,X≈ 100–1000; and (iv) steep−2≳αOX≳−1.7. These results lead to a scenario in which the X-ray emission of hyper-luminous quasars is relatively weaker compared to lower luminosity AGN. Models predict that such an X-ray weakness can be relevant for the acceleration of powerful high-ionization, emission-line-driven winds, which are commonly detected in the UV spectra of WISSH quasars and can, in turn, perturb the X-ray corona and weaken its emission. Accordingly, hyper-luminous quasars represent the ideal laboratory to study the link between the AGN energy output and wind acceleration. Additionally, WISSH quasars exhibit very large SMBH masses (log [MBH/M⊙]≳9.5). This enables a more robust modeling of theΓ–MBHrelation by increasing the statistics at high masses. We derive a flatterΓdependence than previously found over the broad range 5≲log (MBH/M⊙)≲11. Finally, we estimate that only 300 ks observations of X-IFU on boardAthenawill offer a detailed view of the properties of absorption features associated with powerful X-ray SMBH winds for a representative sample of WISSH quasars.
