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

## TL;DR

This study presents detailed X-ray spectral analysis of a high-redshift ultraluminous quasar, revealing its spectral shape, luminosity, and accretion properties, and compares it with other quasars to understand early universe black hole growth.

## Contribution

First detailed XMM-Newton spectral analysis of the ultraluminous quasar SDSS J010013.02+280225.8 at z=6.326, constraining its spectral properties and accretion state.

## Key findings

- Spectral index of Γ = 2.30 ± 0.10.
- Intrinsic 2-10 keV luminosity of 3.14×10^{45} erg/s.
- Sub-Eddington accretion rate inferred.

## 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 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.