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A significant fraction of the most massive stars move through space with ahigh velocity. One of the possible physical explanations is that a supernova ina compact binary system results in a high recoil velocity of the system. If thesystem remains bound, it can be subsequently observed as a spectroscopic binary(SB1), a high-mass X-ray binary, a compact binary, and finally agravitational-wave event. If such a system is traced back to its parentcluster, binary evolution models can be tested in great detail. The Gaia propermotions and parallaxes are used to demonstrate that the high-mass X-ray binaryHD153919/4U 1700-37 originates from NGC6231, the nucleus of the OB associationSco OB1. The O supergiant and its compact companion, of which the physicalnature (a neutron star or a black hole) is unknown, move with a space velocityof 63 km/s with respect to NGC6231. The kinematical age of the system is 2.2Myr. The parallaxes and accurate proper motions in Gaia DR2 were used toperform a membership analysis of NGC 6231. The distance to NGC6231 is 1.63 kpc.Isochrone fitting results in an age of 4.7 Myr. With the identification ofNGC6231 as the parent cluster, the upper limit on the age of the progenitor of4U1700-37 at the moment of the supernova explosion is 3.0 Myr. With theseconstraints, the evolutionary history of the system can be reconstructed withan initial mass of the progenitor of the compact object >60 Msun. Given itscurrent high space velocity and the derived evolutionary history, the compactobject in the system is more likely to have received a large natal kick, whichsuggests that it is more likely a neutron star than a black hole.HD153919/4U1700-37 might be a prototype in the Milky Way for the progenitor ofgravitational wave events such as GW190412

Confirming NGC 6231 as the parent cluster of the runaway high-mass X-ray binary HD 153919/4U 1700-37 with Gaia DR2