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  •   Open Research
  • AUT Faculties
  • Faculty of Design and Creative Technologies (Te Ara Auaha)
  • School of Engineering, Computer and Mathematical Sciences - Te Kura Mātai Pūhanga, Rorohiko, Pāngarau
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Potential Kick Velocity Distribution of Black Hole X-ray Binaries and Implications for Natal Kicks

Atri, P; Miller-Jones, JCA; Bahramian, A; Plotkin, RM; Jonker, PG; Nelemans, G; Maccarone, TJ; Sivakoff, GR; Deller, AT; Chaty, S; Torres, MAP; Horiuchi, S; McCallum, J; Natusch, T; Phillips, CJ; Stevens, J; Weston, S
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http://hdl.handle.net/10292/12805
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Abstract
We use Very Long Baseline Interferometry to measure the proper motions of three black hole X-ray binaries (BHXBs). Using these results together with data from the literature and Gaia-DR2 to collate the best available constraints on proper motion, parallax, distance and systemic radial velocity of 16 BHXBs, we determined their three dimensional Galactocentric orbits. We extended this analysis to estimate the probability distribution for the potential kick velocity (PKV) a BHXB system could have received on formation. Constraining the kicks imparted to BHXBs provides insight into the birth mechanism of black holes (BHs). Kicks also have a significant effect on BH-BH merger rates, merger sites, and binary evolution, and can be responsible for spin-orbit misalignment in BH binary systems. $75\%$ of our systems have potential kicks $>70\,\rm{km~s^{-1}}$. This suggests that strong kicks and hence spin-orbit misalignment might be common among BHXBs, in agreement with the observed quasi-periodic X-ray variability in their power density spectra. We used a Bayesian hierarchical methodology to analyse the PKV distribution of the BHXB population, and suggest that a unimodal Gaussian model with a mean of $107\pm16\,\rm{km~s^{-1}}$ is a statistically favourable fit. Such relatively high PKVs would also reduce the number of BHs likely to be retained in globular clusters. We found no significant correlation between the BH mass and PKV, suggesting a lack of correlation between BH mass and the BH birth mechanism. Our Python code allows the estimation of the PKV for any system with sufficient observational constraints.
Keywords
astro-ph.HE; astro-ph.HE; Astrometry–proper motions–parallaxes–stars: Black hole– stars: Kinematics and dynamics–X-rays: Binaries
Source
arXiv:1908.07199 [astro-ph.HE]
Item Type
Journal Article
Publisher
arXiv
Publisher's Version
https://arxiv.org/abs/1908.07199
Rights Statement
arXiv places no restrictions on whether articles also appear in local institutional repositories. Authors are welcome to download copies of their own articles from arXiv in order to submit to a local repository.

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