XMM–Newton observation of the ultraluminous quasar SDSS J010013.02+280225.8 at redshift 6.326
| Autor: | Feige Wang, Tullia Sbarrato, Long-Long Feng, Xue-Bing Wu, Y. L. Ai, Stephen Walker, Xiaohui Fan, Andrew C. Fabian, Gabriele Ghisellini, Liming Dou |
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| Přispěvatelé: | Fabian, Andrew [0000-0002-9378-4072], Apollo - University of Cambridge Repository, ITA |
| Rok vydání: | 2017 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics 010308 nuclear & particles physics Astrophysics::High Energy Astrophysical Phenomena Member states galaxies: active FOS: Physical sciences Astronomy Astronomy and Astrophysics Quasar Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Astrophysics - Astrophysics of Galaxies 01 natural sciences Redshift galaxies: high-redshift quasars: individual: SDSS J010013.02+280225.8 Space and Planetary Science Basic research Astrophysics of Galaxies (astro-ph.GA) 0103 physical sciences Astrophysics - High Energy Astrophysical Phenomena 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 470:1587-1592 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stx1231 |
| Popis: | 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 ct/ks. In this paper we present results for the quasar from a 65ks XMM-Newton observation, which well constrains its spectral shape. The quasar is clearly detected with a total of $\sim$ 460 net counts in the 0.2-10 keV band. The spectrum is characterised by a simple power-law model with photon index of $\Gamma = 2.30^{+0.10}_{-0.10}$, and the intrinsic 2-10 keV luminosity is $3.14\times10^{45}$ erg $\text{s}^{-1}$. The 1 $\sigma$ upper limit to any intrinsic absorption column density is $N_{H} = 6.07\times 10^{22} {\text{cm}}^{-2}$. No significant iron emission lines were detected. We derive the X-ray-to-optical flux ratio $\alpha_{\text{ox}}$ of $-1.74\pm$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 XMM-Newton observations, which are separated by $\sim$ 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. Comment: 6 pages, 6 figures, accepted by MNRAS |
| Databáze: | OpenAIRE |
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