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We present new observations of the highest-redshift quasar known, ULASJ1120+0641, redshift $z=7.084$, obtained in the optical, at near-, mid-, andfar-infrared wavelengths, and in the sub-mm. We combine these results withpublished X-ray and radio observations to create the multiwavelength spectralenergy distribution (SED), with the goals of measuring the bolometricluminosity $L_{\rm bol}$, and quantifying the respective contributions from theAGN and star formation. We find three components are needed to fit the dataover the wavelength range $0.12-1000\,\mu$m: the unobscured quasar accretiondisk and broad-line region, a dusty clumpy AGN torus, and a cool 47K modifiedblack body to characterise star formation. Despite the low signal-to-noiseratio of the new long-wavelength data, the normalisation of any dusty torusmodel is constrained within $\pm40\%$. We measure a bolometric luminosity$L_{\rm bol}=2.6\pm0.6\times10^{47}\,$erg$\,$s$^{-1}=6.7 \pm1.6\times10^{13}L_{\odot}$, to which the three components contribute$31\%,32\%,3\%$, respectively, with the remainder provided by the extreme UV$<0.12\,\mu$m. We tabulate the best-fit model SED. We use local scalingrelations to estimate a star formation rate (SFR) in the range $60-270\,{\rmM}_\odot$/yr from the [C$\,{\scriptsize \rm II}$] line luminosity and the$158\,\mu$m continuum luminosity. An analysis of the equivalent widths of the[C$\,{\scriptsize \rm II}$] line in a sample of $z>5.7$ quasars suggests thatthese indicators are promising tools for estimating the SFR in high-redshiftquasars in general. At the time observed the black hole was growing in massmore than 100 times faster than the stellar bulge, relative to the mass ratiomeasured in the local universe, i.e. compared to ${M_{\rm BH}}/{M_{\rm bulge}}\simeq 1.4\times10^{-3}$, for ULAS J1120+0641 we measure ${\dot{M}_{\rmBH}}/{\dot{M}_{\rm bulge}} \simeq 0.2$.

The spectral energy distribution of the redshift 7.1 quasar ULAS J1120+0641