On the natal kick of the black hole X-ray binary H 1705–250. (arXiv:2310.11492v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Brown_C/0/1/0/all/0/1">Cordelia Dashwood Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gandhi_P/0/1/0/all/0/1">Poshak Gandhi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_Y/0/1/0/all/0/1">Yue Zhao</a>
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.
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.
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