We report on analysis of properties of the X-ray binary pulsar GRO J1750 - 27 based on X-ray ( Chandra , Swift , and Fermi /GBM ) , and near-infrared ( VVV and UKIDSS surveys ) observations .
An accurate position of the source is determined for the first time and used to identify its infrared counterpart .
Based on the VVV data we investigate the spectral energy distribution ( SED ) of the companion , taking into account a non-standard absorption law in the source direction .
A comparison of this SED with those of known Be/X-ray binaries and early type stars has allowed us to estimate a lower distance limit to the source at > 12 kpc .
An analysis of the observed spin-up torque during a giant outburst in 2015 provides an independent distance estimate of 14 - 22 kpc , and also allows to estimate the magnetic field on the surface of the neutron star at B \simeq ( 3.5 - 4.5 ) \times 10 ^ { 12 } G. The latter value is in agreement with the possible transition to the propeller regime , a strong hint for which was revealed by Swift /XRT and Chandra .
We conclude , that GRO J1750 - 27 is located far behind the Galactic Center , which makes it one of the furthest Galactic X-ray binaries known .