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When a compact object is formed, an impulse (kick) will be imparted to thesystem by the mass lost during the core-collapse supernova (SN). A number ofother mechanisms may impart an additional kick on the system, although evidencefor these natal kicks in black hole systems remains limited. Updated Gaiaastrometry has recently identified a number of high peculiar velocity (inexcess of Galactic motion) compact objects. Here, we focus on the black holelow-mass X-ray binary H 1705--250, which has a peculiar velocity$\upsilon_{\mathrm{pec}}\,=\,221^{+101}_{-108}\,\mathrm{km}\,\mathrm{s}^{-1}$.Using population synthesis to reconstruct its evolutionary history (assumingformation via isolated binary evolution within the Galactic plane), weconstrain the properties of the progenitor and pre-SN orbit. The magnitude of akick solely due to mass loss is found to be$\sim\,30\,\mathrm{km}\,\mathrm{s}^{-1}$, which cannot account for the highpresent-day peculiar motion. We therefore deduce that the black hole receivedan additional natal kick at formation, and place limits on its magnitude,finding it to be $\sim\,295\,\mathrm{km}\,\mathrm{s}^{-1}$ (minimum$90\,\mathrm{km}\,\mathrm{s}^{-1}$). This furthers the argument that thesekicks are not limited to neutron stars.

On the natal kick of the black hole X-ray binary H 1705--250