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IGR J17062-6143 is an ultra-compact X-ray binary (UCXB) with an orbitalperiod of 37.96 min. It harbours a millisecond X-ray pulsar that is spinning at163 Hz and and has continuously been accreting from its companion star since2006. Determining the composition of the accreted matter in UCXBs is of highinterest for studies of binary evolution and thermonuclear burning on thesurface of neutron stars. Here, we present a multi-wavelength study of IGRJ17062-6143 aimed to determine the detailed properties of its accretion discand companion star. The multi-epoch photometric UV to near-infrared spectralenergy distribution (SED) is consistent with an accretion disc$F_{\nu}\propto\nu^{1/3}$. The SED modelling of the accretion disc allowed usto estimate an outer disc radius of $R_{out}=2.2^{+0.9}_{-0.4} \times 10^{10}$cm and a mass-transfer rate of $\dot{m}=1.8^{+1.8}_{-0.5}\times10^{-10}$M$_{\odot}$ yr$^{-1}$. Comparing this with the estimated mass-accretion rateinferred from its X-ray emission suggests that $\gtrsim$90% of the transferredmass is lost from the system. Moreover, our SED modelling shows that thethermal emission component seen in the X-ray spectrum is highly unlikely fromthe accretion disc and must therefore represent emission from the surface ofthe neutron star. Our low-resolution optical spectrum revealed a blue continuumand no emission lines, i.e. lacking H and He features. Based on the currentdata we cannot conclusively identify the nature of the companion star, but wemake recommendations for future study that can distinguish between thedifferent possible evolution histories of this X-ray binary. Finally, wedemonstrate how multiwavelength observations can be effectively used to findmore UCXBs among the LMXBs.

Multiwavelength characterisation of the accreting millisecond X-ray pulsar and ultra-compact binary IGR J17062-6143