Recoiling Black Holes in Quasars

Bonning, E. W.; Shields, G. A.; Salviander, S.

doi:10.1086/521674

Cited by 131 publications

(188 citation statements)

References 48 publications

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“…Notably, it has been successfully applied to many-black-hole spacetimes [27,28], and to black-hole-neutron star evolutions [29,30,31,32]. Similarly, the recent discovery of very large merger recoil kicks [33,34,35,36,37,38,39,40] has had a great impact in the astrophysical community, with several groups now seeking for observational traces of such high speed holes as the byproduct of galaxy collisions [41,42,43,44].…”

Section: Introductionmentioning

confidence: 99%

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

2008

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We evolve equal-mass, equal-spin black-hole binaries with specific spins of a/mH ∼ 0.925, the highest spins simulated thus far and nearly the largest possible for Bowen-York black holes, in a set of configurations with the spins counter-aligned and pointing in the orbital plane, which maximizes the recoil velocities of the merger remnant, as well as a configuration where the two spins point in the same direction as the orbital angular momentum, which maximizes the orbital hang-up effect and remnant spin. The coordinate radii of the individual apparent horizons in these cases are very small and the simulations require very high central resolutions (h ∼ M/320). We find that these highly spinning holes reach a maximum recoil velocity of ∼ 3300 km s −1 (the largest simulated so far) and, for the hangup configuration, a remnant spin of a/mH ∼ 0.922. These results are consistent with our previous predictions for the maximum recoil velocity of ∼ 4000 km s −1 and remnant spin; the latter reinforcing the prediction that cosmic censorship is not violated by merging highlyspinning black-hole binaries. We also numerically solve the initial data for, and evolve, a single maximal-Bowen-York-spin black hole, and confirm that the 3-metric has an O(r −2 ) singularity at the puncture, rather than the usual O(r −4 ) singularity seen for non-maximal spins.

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Section: Introductionmentioning

confidence: 99%

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

2008

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“…These breakthroughs have also influenced the development of data analysis techniques through the matching of post-Newtonian to fully-numerical waveforms [16,17,18]. Similarly, the recent discovery of very large merger recoil kicks [19,20,21,22,23,24,25,26] has had a great impact in the astrophysical community, with several groups now seeking for observational traces of such high speed holes as the byproduct of galaxy collisions [27,28]. In this letter, we continue our quest to discover new astrophysical consequences of black-hole interactions by simulating close encounters of three black holes to see the different behaviors introduced by the finite size of the holes, their nonlinear interactions, and the radiation of gravitational waves, as described by General Relativity.…”

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confidence: 99%

Close encounters of three black holes

2008

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We present the first fully relativistic longterm numerical evolutions of three equal-mass black holes in a system consisting of a third black hole in a close orbit about a black-hole binary. We find that these close-three-black-hole systems have very different merger dynamics from black-hole binaries. In particular, we see complex trajectories, a redistribution of energy that can impart substantial kicks to one of the holes, distinctive waveforms, and suppression of the emitted gravitational radiation. We evolve two such configurations and find very different behaviors. In one configuration the binary is quickly disrupted and the individual holes follow complicated trajectories and merge with the third hole in rapid succession, while in the other, the binary completes a half-orbit before the initial merger of one of the members with the third black hole, and the resulting two-black-hole system forms a highly elliptical, well separated binary that shows no significant inspiral for (at least) the first t ∼ 1000M of evolution. Introduction: The recent dramatic breakthroughs in the numerical techniques to evolve black-hole-binary spacetimes [1, 2, 3] has led to rapid advancements in our understanding of black-hole physics. Notable among these advancements are developments in mathematical relativity, including systems of PDEs and gauge choices [4,5,6], the exploration of the cosmic censorship [7,8,9,10,11], and the application of isolated horizon formulae [8,9,12,13,14,15]. These breakthroughs have also influenced the development of data analysis techniques through the matching of post-Newtonian to fully-numerical waveforms [16,17,18]. Similarly, the recent discovery of very large merger recoil kicks [19,20,21,22,23,24,25,26] has had a great impact in the astrophysical community, with several groups now seeking for observational traces of such high speed holes as the byproduct of galaxy collisions [27,28]. In this letter, we continue our quest to discover new astrophysical consequences of black-hole interactions by simulating close encounters of three black holes to see the different behaviors introduced by the finite size of the holes, their nonlinear interactions, and the radiation of gravitational waves, as described by General Relativity. We find that the three-body relativistic problem shows far richer dynamics than the two-body problem, akin to the rich three-body dynamics in Newtonian gravity, but with added complexity due to mergers.

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“…The quasar SDSSJ0927+2943 (Komossa et al 2008;KZL08 hereafter) shows the characteristic optical signatures of a recoiling SMBH, which were predicted by Bonning et al (2007): its broad emission lines are shifted by 2650 km s −1 with respect to its narrow emission lines, the broad lines are symmetric, the broad Mg ii line shows the same shift as the broad Balmer lines, and the narrow emission lines lack ionization stratification as expected if the accreting SMBH is no longer at the center of the system (KZL08). † Its unique properties make SDSSJ0927+2943 an excellent candidate for a recoiling SMBH.…”

Section: The Candidate Recoiling Smbh Sdssj0927+2943 and X-ray Followmentioning

confidence: 85%

“…Recoiling SMBHs will therefore appear as AGN which have their broad emission lines kinematically shifted by up to ∼ 3800 km s −1 with respect to their NLRs. Bonning et al (2007) formulated several criteria, how a recoiling SMBH should appear spectroscopically. Apart from (1) the kinematic shift of the BLR, a candidate ejected SMBH should (2) exhibit symmetric broad-line profiles, it should (3) lack stratification of high-versus low-ionization narrow emission lines, and it should (4) not show any shift between broad Mg ii and the broad Balmer lines †.…”

Section: Emission-line Signatures Of Recoiling Smbhsmentioning

confidence: 99%

Electromagnetic Signatures of Recoiling Black Holes

Komossa¹

2009

Proc. IAU

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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 anisotropic emission of gravitational waves, leading to long-lived oscillations of the SMBHs in galaxy cores and even SMBH ejections from their host galaxies. Observationally, accreting recoiling SMBHs would appear as quasars spatially and/or kinematically offset from their host galaxies. The presence of these "kicks" and "superkicks" has a wide range of exciting astrophysical implications which only now are beginning to be explored, including consequences for black hole and galaxy growth at the epoch of structure formation, modes of feedback, unified models of AGN, and the number of obscured AGN. SMBH recoil oscillations beyond the torus scale can be on the order of a quasar lifetime, thus potentially affecting a large fraction of the quasar population. We discuss how this might explain the long-standing puzzle of a deficiency of obscured type 2 quasars at high luminosities. Observational signatures of recoiling SMBHs are discussed and results from follow-up studies of the candidate recoiling SMBH SDSSJ0927+2943 are presented.

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Recoiling Black Holes in Quasars

Cited by 131 publications

References 48 publications

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

Close encounters of three black holes

Electromagnetic Signatures of Recoiling Black Holes

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