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Title:
The formation of the black hole in the X-ray binary system V404 Cyg
Authors:
Miller-Jones, J. C. A.; Jonker, P. G.; Nelemans, G.; Portegies Zwart, S.; Dhawan, V.; Brisken, W.; Gallo, E.; Rupen, M. P.
Affiliation:
AA(NRAO Headquarters, 520 Edgemont Road, Charlottesville, VA 22903, USA), AB(SRON, Netherlands Institute for Space Research, 3584 CA Utrecht, the Netherlands; Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), AC(Department of Astrophysics, IMAPP, Radboud University, Toernooiveld 1, 6525 ED, Nijmegen, the Netherlands), AD(Astronomical Institute `Anton Pannekoek', University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, the Netherlands; Section Computational Science, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, the Netherlands), AE(NRAO, Array Operations Center, 1003 Lopezville Road, Socorro, NM 87801, USA), AF(NRAO, Array Operations Center, 1003 Lopezville Road, Socorro, NM 87801, USA), AG(Physics Department, Broida Hall, University of California, Santa Barbara, CA 93106, USA), AH(NRAO, Array Operations Center, 1003 Lopezville Road, Socorro, NM 87801, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 394, Issue 3, pp. 1440-1448. (MNRAS Homepage)
Publication Date:
04/2009
Origin:
MNRAS
MNRAS Keywords:
astrometry , stars: individual: V404 Cyg , stars: kinematics , stars: supernovae: general , radio continuum: stars , X-rays: binaries
DOI:
10.1111/j.1365-2966.2009.14404.x
Bibliographic Code:
2009MNRAS.394.1440M

Abstract

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 +/- 0.3masyr-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 47-102kms-1, with a best-fitting value of 64kms-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 (~11Msolar) was lost, giving rise to a symmetric Blaauw kick of up to ~65kms-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 ~9Msolar, since when it has accreted 0.5-1.5Msolar from its companion.
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