Effects of post-Newtonian Spin Alignment on the Distribution of Black-Hole Recoils

Abstract

Recent numerical relativity simulations have shown that the final black hole produced in a binary merger can recoil with a velocity as large as 5,000 km/s. Because of enhanced gravitational-wave emission in the so-called "hang-up" configurations, this maximum recoil occurs when the black-hole spins are partially aligned with the orbital angular momentum. We revisit our previous statistical analysis of post-Newtonian evolutions of black-hole binaries in the light of these new findings. We demonstrate that despite these new configurations with enhanced recoil velocities, spin alignment during the post-Newtonian stage of the inspiral will still significantly suppress (or enhance) kick magnitudes when the initial spin of the more massive black hole is more (or less) closely aligned with the orbital angular momentum than that of the smaller hole. We present a preliminary study of how this post-Newtonian spin alignment affects the ejection probabilities of supermassive black holes from their host galaxies with astrophysically motivated mass ratio and initial spin distributions. We find that spin alignment suppresses (enhances) ejection probabilities by ~ 40% (20%) for an observationally motivated mass-dependent galactic escape velocity, and by an even greater amount for a constant escape velocity of 1,000 km/s. Kick suppression is thus at least a factor two more efficient than enhancement.

12 pages, 4 figures, 1 table. Added a second panel to figure 1. Minor changes to the text in response to the referee's comments

References in corpus (14)

• Large Merger Recoils and Spin Flips From Generic Black-Hole Binaries
• Supermassive black hole formation during the assembly of pre-galactic discs
• Total recoil: the maximum kick from nonspinning black-hole binary inspiral
• Supermassive recoil velocities for binary black-hole mergers with antialigned spins
• The star formation histories of galaxies in the Sloan Digital Sky Survey
• Alignment of the spins of supermassive black holes prior to coalescence
• The Evolution of Black Hole Mass and Spin in Active Galactic Nuclei
• Ejection of Supermassive Black Holes from Galaxy Cores
• Reconstructing the massive black hole cosmic history through gravitational waves
• Relativistic Suppression of Black Hole Recoils
• Binary black hole merger: symmetry and the spin expansion
• Final spins from the merger of precessing binary black holes
• The spin expansion for binary black hole merger: new predictions and future directions
• Constraining properties of the black hole population using LISA

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