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http://hdl.handle.net/20.500.12386/26883
Titolo: | XMM-Newton observation of the ultraluminous quasar SDSS J010013.02+280225.8 at redshift 6.326 | Autori: | Ai, Yanli Fabian, A. C. Fan, Xiaohui Walker, S. A. GHISELLINI, Gabriele Sbarrato, Tullia Dou, Liming Wang, Feige Wu, Xue-Bing Feng, Longlong |
Data pubblicazione: | 2017 | Rivista: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Numero: | 470 | Fascicolo: | 2 | Da pagina:: | 1587 | Abstract: | A brief Chandra observation of the ultraluminous quasar SDSS J010013.02+280225.8 at redshift 6.326 showed it to be a relatively bright, soft X-ray source with a count rate of about 1 count ks<SUP>-1</SUP>. In this article, we present results for the quasar from a 65-ks XMM-Newton observation, which constrains its spectral shape well. The quasar is clearly detected with a total of ∼460 net counts in the 0.2-10 keV band. The spectrum is characterized by a simple power-law model with a photon index of Γ = 2.30^{+0.10}_{-0.10} and the intrinsic 2-10 keV luminosity is 3.14 × 10<SUP>45</SUP> erg s<SUP>-1</SUP>. The 1σ upper limit to any intrinsic absorption column density is N<SUB>H</SUB> = 6.07 × 10<SUP>22</SUP> cm<SUP>-2</SUP>. No significant iron emission lines were detected. We derive an X-ray-to-optical flux ratio α<SUB>ox</SUB> of -1.74 ± 0.01, consistent with the values found in other quasars of comparable ultraviolet luminosity. We did not detect significant flux variations either in the XMM-Newton exposure or between XMM-Newton and Chandra observations, which are separated by ∼8 months. The X-ray observation enables the bolometric luminosity to be calculated after modelling the spectral energy distribution: the accretion rate is found to be sub-Eddington. | URI: | http://hdl.handle.net/20.500.12386/26883 | URL: | https://academic.oup.com/mnras/article-abstract/470/2/1587/3906739?redirectedFrom=fulltext | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stx1231 | Bibcode ADS: | 2017MNRAS.470.1587A | Fulltext: | open |
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