A Recoiling Supermassive Black Hole in the Quasar SDSS J092712.65+294344.0?

@article{Komossa2008ARS,
  title={A Recoiling Supermassive Black Hole in the Quasar SDSS J092712.65+294344.0?},
  author={Stefanie Komossa and H. Y. Zhou and H. L. Lu},
  journal={The Astrophysical Journal Letters},
  year={2008},
  volume={678},
  pages={L81 - L84}
}
We present SDSS J092712.65+294344.0 as the best candidate to date for a recoiling supermassive black hole (SMBH). SDSS J0927+2943 shows an exceptional optical emission-line spectrum with two sets of emission lines: one set of very narrow emission lines, and a second set of broad Balmer and broad high-ionization forbidden lines which are blueshifted by 2650 km s−1 relative to the set of narrow emission lines. This observation is most naturally explained if the SMBH was ejected from the core of… 

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References

SHOWING 1-10 OF 47 REFERENCES

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

Constraints from Gravitational Recoil on the Growth of Supermassive Black Holes at High Redshift

Recent studies have suggested that during their coalescence, binary supermassive black holes (SMBHs) experience typical gravitational recoil velocities that may be as large as ≳100 km s-1. These

Quasars at z = 6: The Survival of the Fittest

The Sloan Digital Sky Survey has detected luminous quasars at very high redshift, z > 6. Follow-up observations indicate that at least some of these quasars are powered by supermassive black holes

The nature of the HE0450−2958 system

Magain et al. argued that the host galaxy of the quasar in HE0450−2958 is substantially underluminous given the quasar brightness. Using kinematical information from the spectra of the quasar and the

Early Reionization by Miniquasars

Motivated by the recent detection by the Wilkinson Microwave Anisotropy Probe of a large optical depth to Thomson scattering, implying a very early reionization epoch, we assess a scenario where the

Fe II Emission in 14 Low-Redshift Quasars. I. Observations

We present the spectra of 14 quasars with a wide coverage of rest wavelengths from 1000 to 7300 Å. The redshift ranges from z = 0.061 to 0.555 and the luminosity from MB = -22.69 to -26.32. These

Observable signatures of a black hole ejected by gravitational-radiation recoil in a galaxy merger.

  • A. Loeb
  • Physics
    Physical review letters
  • 2007
TLDR
The circumstances resulting from a gas-rich galaxy merger under which the ejected BH would carry an accretion disk and be observable are examined.

Possible evidence for the ejection of a supermassive black hole from an ongoing merger of galaxies

Attempts of Magain et al. to detect the host galaxy of the bright quasi-stellar object (QSO) HE0450-2958 have not been successful. We suggest that the supermassive black hole (SMBH) powering the QSO

The effect of gravitational recoil on black holes forming in a hierarchical universe

Galactic bulges are known to harbour central black holes whose mass is tightly correlated with the stellar mass and velocity dispersion of the bulge. In a hierarchical universe, galaxies are built up

Extreme recoils: impact on the detection of gravitational waves from massive black hole binaries

Recent numerical simulations of the coalescence of highly spinning massive black hole binaries (MBHBs) suggest that the remnant can suffer a recoil velocity of the order of few thousand km s−1. We