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On the mass radiated by coalescing black-hole binaries: Erratum ApJ, 2012, 758, 63

MPS-Authors

Morozova,  Viktoriya
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Rezzolla,  Luciano
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Citation

Barausse, E., Morozova, V., & Rezzolla, L. (2014). On the mass radiated by coalescing black-hole binaries: Erratum ApJ, 2012, 758, 63. The Astrophysical Journal, 786(1): 76. doi:10.1088/0004-637X/786/1/76.


Cite as: http://hdl.handle.net/11858/00-001M-0000-001A-10B8-F
Abstract
We derive an analytic phenomenological expression that predicts the final mass of the black-hole remnant resulting from the merger of a generic binary system of black holes on quasi-circular orbits. Besides recovering the correct test-particle limit for extreme mass-ratio binaries, our formula reproduces well the results of all the numerical-relativity simulations published so far, both when applied at separations of a few gravitational radii, and when applied at separations of tens of thousands of gravitational radii. These validations make our formula a useful tool in a variety of contexts ranging from gravitational-wave physics to cosmology. As representative examples, we first illustrate how it can be used to decrease the phase error of the effective-one-body waveforms during the ringdown phase. Second, we show that, when combined with the recently computed self-force correction to the binding energy of nonspinning black-hole binaries, it provides an estimate of the energy emitted during the merger and ringdown. Finally, we use it to calculate the energy radiated in gravitational waves by massive black-hole binaries as a function of redshift, using different models for the seeds of the black-hole population.