Ejection of Supermassive Black Holes from Galaxy Cores

  title={Ejection of Supermassive Black Holes from Galaxy Cores},
  author={Alessia Gualandris and David Merritt},
  journal={The Astrophysical Journal},
  pages={780 - 797}
Recent numerical relativity simulations have shown that the emission of gravitational waves during the merger of two supermassive black holes (SMBHs) delivers a kick to the final hole, with a magnitude as large as 4000 km s−1. We study the motion of SMBHs ejected from galaxy cores by such kicks and the effects on the stellar distribution using high-accuracy direct N-body simulations. Following the kick, the motion of the SMBH exhibits three distinct phases. (1) The SMBH oscillates with… 

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Electromagnetic Signatures of Recoiling Black Holes

    S. Komossa
    Proceedings of the International Astronomical Union
  • 2009
Abstract Recent numerical relativity simulations predict that coalescing supermassive black holes (SMBHs) can receive kick velocities up to several thousands of kilometers per second due to


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Recoiling Black Holes: Electromagnetic Signatures, Candidates, and Astrophysical Implications

Supermassive black holes (SMBHs) may not always reside right at the centers of their host galaxies. This is a prediction of numerical relativity simulations, which imply that the newly formed single


The coalescence of a binary black hole can be accompanied by a large gravitational recoil due to anisotropic emission of gravitational waves. A recoiling supermassive black hole (SBH) can

The influence of Massive Black Hole Binaries on the Morphology of Merger Remnants

Massive black hole (MBH) binaries, formed as a result of galaxy mergers, are expected to harden by dynamical friction and three-body stellar scatterings, until emission of gravitational waves (GWs)

Imprints of recoiling massive black holes on the hot gas of early-type galaxies

Anisotropic gravitational radiation from a coalescing black hole (BH) binary is known to impart recoil velocities of up to ∼1000 km s -1 to the remnant BH. In this context, we study the motion of a

Spin, Accretion, and the Cosmological Growth of Supermassive Black Holes

If supermassive black holes (SMBHs) are the energy sources that power quasars and active galactic nuclei (AGNs), then QSO SDSS 1148+5251, the quasar with the highest redshift (zQSO = 6.43), hosts an

Formation of Galactic Nuclei

We investigate a model in which galactic nuclei form via the coalescence of preexisting stellar systems containing supermassive black holes. Merger simulations are carried out using N-body algorithms

Mass Deficits, Stalling Radii, and the Merger Histories of Elliptical Galaxies

A binary supermassive black hole leaves an imprint on a galactic nucleus in the form of a "mass deficit," a decrease in the mass of the nucleus due to ejection of stars by the binary. The magnitude

The Distribution of Recoil Velocities from Merging Black Holes

We calculate the linear momentum flux from merging black holes (BHs) with arbitrary masses and spin orientations, using the effective-one-body (EOB) model. This model includes an analytic description

Getting a Kick Out of Numerical Relativity

Recent developments in numerical relativity have made it possible to reliably follow the coalescence of two black holes from near the innermost stable circular orbit to final ringdown. This opens up

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Using high resolution N-body simulations of stellar disks embedded in cosmologically motivated dark matter halos, we study the evolution of bars and the transfer of angular momentum between halos and

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Gravitational waves from the coalescence of binary black holes carry away linear momentum, causing center of mass recoil. This "radiation rocket" effect has important implications for systems with

Core Formation in Galactic Nuclei due to Recoiling Black Holes

Anisotropic gravitational radiation from a coalescing black hole binary can impart a recoil velocity of up to several hundred kilometers per second to the remnant black hole. We examine the effects

Recoiling Black Holes in Quasars

Recent simulations of merging black holes with spin give recoil velocities from gravitational radiation up to several thousand kilometers per second. A recoiling supermassive black hole can retain

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New measurements of the stellar-mass deficits at the centers of luminous elliptical galaxies are presented. These were derived considering the following observational facts. First, "core" galaxies,