Context :

Aims : We aim at probing the emission mechanism of the accreting super massive black holes in the high redshift Universe .

Methods : We study the X-ray spectrum of ULAS1120+0641 , the highest redshift quasar detected so far at z=7.085 , which has been deeply observed ( 340 ks ) by XMM-Newton .

Results : Despite the long integration time the spectral analysis is limited by the poor statistics , with only 150 source counts being detected .
We measured the spectrum in the 2-80 keV rest-frame ( 0.3-10 keV observed ) energy band .
Assuming a simple power law model we find a photon index of 2.0 \pm 0.3 and a luminosity of 6.7 \pm 0.3 10 ^ { 44 } erg s ^ { -1 } in the 2-10 keV band , while the intrinsic absorbing column can be only loosely constrained ( N _ { H } < 10 ^ { 23 } cm ^ { -2 } ) .
Combining our measure with published data , we calculate that the X-ray-to-optical spectral index \alpha _ { OX } is1.8 \pm 0.1 , in agreement with the \alpha _ { OX } -UV luminosity correlation valid for lower redshift quasars .

Conclusions : We expanded to high energies the coverage of the spectral energy distribution of ULAS1120+0641 .
This is the second time that a z > 6 quasar has been investigated through a deep X-ray observation .
In agreement with previous studies of z \sim 6 AGN samples , we do not find any hint of evolution in the broadband energy distribution .
Indeed from our dataset ULAS 1120+0641 is indistinguishable from the population of optically bright quasar at lower redshift .