{ "id": "2310.11492", "version": "v1", "published": "2023-10-17T18:00:02.000Z", "updated": "2023-10-17T18:00:02.000Z", "title": "On the natal kick of the black hole X-ray binary H 1705--250", "authors": [ "Cordelia Dashwood Brown", "Poshak Gandhi", "Yue Zhao" ], "comment": "MNRAS in press", "categories": [ "astro-ph.HE", "astro-ph.SR" ], "abstract": "When a compact object is formed, an impulse (kick) will be imparted to the system by the mass lost during the core-collapse supernova (SN). A number of other mechanisms may impart an additional kick on the system, although evidence for these natal kicks in black hole systems remains limited. Updated Gaia astrometry has recently identified a number of high peculiar velocity (in excess of Galactic motion) compact objects. Here, we focus on the black hole low-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 (assuming formation via isolated binary evolution within the Galactic plane), we constrain the properties of the progenitor and pre-SN orbit. The magnitude of a kick solely due to mass loss is found to be $\\sim\\,30\\,\\mathrm{km}\\,\\mathrm{s}^{-1}$, which cannot account for the high present-day peculiar motion. We therefore deduce that the black hole received an 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 these kicks are not limited to neutron stars.", "revisions": [ { "version": "v1", "updated": "2023-10-17T18:00:02.000Z" } ], "analyses": { "keywords": [ "black hole x-ray binary", "natal kick", "hole systems remains", "black hole low-mass x-ray binary", "compact object" ], "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable" } } }