XMM-Newton observation of the ultraluminous quasar SDSS J010013.02+280225.8 at redshift 6.326

Yanli Ai, A. C. Fabian, Xiaohui Fan, S. A. Walker, G. Ghisellini, T. Sbarrato, Liming Dou, Feige Wang, Wu Xue-Bing Wu, Longlong Feng

Research output: Contribution to journalArticle

1 Citation (Scopus)

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-1. 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 × 1045 erg s-1. The 1σ upper limit to any intrinsic absorption column density is NH = 6.07 × 1022 cm-2. No significant iron emission lines were detected. We derive an X-rayto- optical flux ratio αox 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.

Original languageEnglish (US)
Article numberstx1231
Pages (from-to)1587-1592
Number of pages6
JournalMonthly Notices of the Royal Astronomical Society
Volume470
Issue number2
DOIs
StatePublished - Sep 11 2017

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XMM-Newton telescope
quasars
newton
luminosity
erg
power law
spectral energy distribution
accretion
iron
x rays
modeling
energy
photons
rate

Keywords

  • Galaxies: active
  • Galaxies: high-redshift
  • Quasars: individual: SDSS J010013.02+280225.8

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

XMM-Newton observation of the ultraluminous quasar SDSS J010013.02+280225.8 at redshift 6.326. / Ai, Yanli; Fabian, A. C.; Fan, Xiaohui; Walker, S. A.; Ghisellini, G.; Sbarrato, T.; Dou, Liming; Wang, Feige; Xue-Bing Wu, Wu; Feng, Longlong.

In: Monthly Notices of the Royal Astronomical Society, Vol. 470, No. 2, stx1231, 11.09.2017, p. 1587-1592.

Research output: Contribution to journalArticle

Ai, Y, Fabian, AC, Fan, X, Walker, SA, Ghisellini, G, Sbarrato, T, Dou, L, Wang, F, Xue-Bing Wu, W & Feng, L 2017, 'XMM-Newton observation of the ultraluminous quasar SDSS J010013.02+280225.8 at redshift 6.326', Monthly Notices of the Royal Astronomical Society, vol. 470, no. 2, stx1231, pp. 1587-1592. https://doi.org/10.1093/mnras/stx1231
Ai, Yanli ; Fabian, A. C. ; Fan, Xiaohui ; Walker, S. A. ; Ghisellini, G. ; Sbarrato, T. ; Dou, Liming ; Wang, Feige ; Xue-Bing Wu, Wu ; Feng, Longlong. / XMM-Newton observation of the ultraluminous quasar SDSS J010013.02+280225.8 at redshift 6.326. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 470, No. 2. pp. 1587-1592.
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AU - Walker, S. A.

AU - Ghisellini, G.

AU - Sbarrato, T.

AU - Dou, Liming

AU - Wang, Feige

AU - Xue-Bing Wu, Wu

AU - Feng, Longlong

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AB - 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-1. 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 × 1045 erg s-1. The 1σ upper limit to any intrinsic absorption column density is NH = 6.07 × 1022 cm-2. No significant iron emission lines were detected. We derive an X-rayto- optical flux ratio αox 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.

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