TY - JOUR
T1 - The formation of the black hole in the X-ray binary system V404 Cyg
AU - Miller-Jones, J. C.A.
AU - Jonker, P. G.
AU - Nelemans, G.
AU - Portegies Zwart, S.
AU - Dhawan, V.
AU - Brisken, W.
AU - Gallo, E.
AU - Rupen, M. P.
PY - 2009/4
Y1 - 2009/4
N2 - Using new and archival radio data, we have measured the proper motion of the black hole X-ray binary V404 Cyg to be 9.2 ± 0.3 mas yr-1. Combined with the systemic radial velocity from the literature, we derive the full three-dimensional heliocentric space velocity of the system, which we use to calculate a peculiar velocity in the range 47-102 km s-1, with a best-fitting value of 64 km s-1. We consider possible explanations for the observed peculiar velocity and find that the black hole cannot have formed via direct collapse. A natal supernova is required, in which either significant mass (∼11 M⊙) was lost, giving rise to a symmetric Blaauw kick of up to ∼65 km s-1, or, more probably, asymmetries in the supernova led to an additional kick out of the orbital plane of the binary system. In the case of a purely symmetric kick, the black hole must have been formed with a mass ∼9 M⊙, since when it has accreted 0.5-1.5 M⊙ from its companion.
AB - Using new and archival radio data, we have measured the proper motion of the black hole X-ray binary V404 Cyg to be 9.2 ± 0.3 mas yr-1. Combined with the systemic radial velocity from the literature, we derive the full three-dimensional heliocentric space velocity of the system, which we use to calculate a peculiar velocity in the range 47-102 km s-1, with a best-fitting value of 64 km s-1. We consider possible explanations for the observed peculiar velocity and find that the black hole cannot have formed via direct collapse. A natal supernova is required, in which either significant mass (∼11 M⊙) was lost, giving rise to a symmetric Blaauw kick of up to ∼65 km s-1, or, more probably, asymmetries in the supernova led to an additional kick out of the orbital plane of the binary system. In the case of a purely symmetric kick, the black hole must have been formed with a mass ∼9 M⊙, since when it has accreted 0.5-1.5 M⊙ from its companion.
KW - Astrometry
KW - Radio continuum: stars
KW - Stars: individual: V404 Cyg
KW - Stars: kinematics
KW - Stars: supernovae: general
KW - X-rays: binaries
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U2 - 10.1111/j.1365-2966.2009.14404.x
DO - 10.1111/j.1365-2966.2009.14404.x
M3 - Article
AN - SCOPUS:63549100171
SN - 0035-8711
VL - 394
SP - 1440
EP - 1448
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -