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http://hdl.handle.net/20.500.12386/32223
Title: | The most luminous blue quasars at 3.0 < z < 3.3: II. C IV /X-ray emission and accretion disc physics | Authors: | Lusso, E. NARDINI, EMANUELE Bisogni, Susanna Risaliti, G. GILLI, Roberto Richards, G. T. Salvestrini, F. Vignali, C. Bargiacchi, G. Civano, F. Elvis, M. Fabbiano, G. Marconi, Alessandro Sacchi, A. Signorini, M. |
Issue Date: | 2021 | Journal: | ASTRONOMY & ASTROPHYSICS | Number: | 653 | First Page: | A158 | Abstract: | We analyse the properties of the high-ionisation C IVλ1549 broad emission line in connection with the X-ray emission of 30 bright, optically selected quasars at z 3.0-3.3 with pointed XMM-Newton observations, which were selected to test the suitability of active galactic nuclei as cosmological tools. In our previous work, we found that a large fraction (≈25%) of the quasars in this sample are X-ray under-luminous by factors of > 3-10. As absorbing columns of 1023 cm-2 can be safely ruled out, their weakness is most likely intrinsic. Here we explore possible correlations between the UV and X-ray features of these sources to investigate the origin of X-ray weakness with respect to X-ray-normal quasars at similar redshifts. We fit the UV spectra from the Sloan Digital Sky Survey of the quasars in our sample and analyse their C IV properties - for example equivalent width (EW) and line peak velocity (υpeak) - as a function of the X-ray photon index and 2-10 keV flux. We confirm the statistically significant trends of C IVυpeak and EW with UV luminosity at 2500 Å for both X-ray-weak and X-ray-normal quasars, as well as the correlation between X-ray weakness (parametrised through Δαox) and C IV EW. In contrast to some recent work, we do not observe any clear relation between the 2-10 keV luminosity and υpeak. We find a statistically significant correlation between the hard X-ray flux and the integrated C IV flux for X-ray-normal quasars, which extends across more than three (two) decades in C IV (X-ray) luminosity, whilst X-ray-weak quasars deviate from the main trend by more than 0.5 dex. We argue that X-ray weakness might be interpreted in a starved X-ray corona picture associated with an ongoing disc-wind phase. If the wind is ejected in the vicinity of the black hole, the extreme-UV radiation that reaches the corona will be depleted, depriving the corona of seed photons and generating an X-ray-weak quasar. Nonetheless, at the largest UV luminosities (> 1047 erg s-1) there will still be an ample reservoir of ionising photons that can explain the 'excess' C IV emission observed in the X-ray-weak quasars with respect to normal sources of similar X-ray luminosities. | URI: | http://hdl.handle.net/20.500.12386/32223 | URL: | https://www.aanda.org/articles/aa/full_html/2021/09/aa41356-21/aa41356-21.html https://api.elsevier.com/content/abstract/scopus_id/85116333857 |
ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/202141356 | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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Lusso+21.pdf | Pdf editoriale | 6.23 MB | Adobe PDF | View/Open |
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