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

##### Fulltext (public)

ApJ_786_1_76.pdf

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##### Supplementary Material (public)

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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.