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We report on analysis of properties of the X-ray binary pulsar GROJ1750-27based on X-ray (Chandra, Swift, and Fermi/GBM), and near-infrared (VVV andUKIDSS surveys) observations. An accurate position of the source is determinedfor the first time and used to identify its infrared counterpart. Based on theVVV data we investigate the spectral energy distribution (SED) of thecompanion, taking into account a non-standard absorption law in the sourcedirection. A comparison of this SED with those of known Be/X-ray binaries andearly type stars has allowed us to estimate a lower distance limit to thesource at $>12$ kpc. An analysis of the observed spin-up torque during a giantoutburst in 2015 provides an independent distance estimate of $14-22$ kpc, andalso allows to estimate the magnetic field on the surface of the neutron starat $B\simeq(3.5-4.5)\times10^{12}$ G. The latter value is in agreement with thepossible transition to the propeller regime, a strong hint for which wasrevealed by Swift/XRT and Chandra. We conclude that GROJ1750-27 is located farbehind the Galactic Center, which makes it one of the furthest Galactic X-raybinaries known.

GROJ1750-27: a neutron star far behind the Galactic Center switching into the propeller regime