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Gravitational-wave data analysis using binary black-hole waveforms

P. Ajith
(
- Hannover, Max Planck Inst. Grav. and
- Hannover U.
)

Dec, 2007

8 pages

Part of Proceedings, 18th International Conference on General Relativity and Gravitation (GRG18) and 7th Edoardo Amaldi Conference on Gravitational Waves (Amaldi7), Sydney, Australia, July 2007

Published in:

Class.Quant.Grav. 25 (2008) 114033

Contribution to:

- GR18 and
- Amaldi7

e-Print:

0712.0343 [gr-qc]

DOI:

10.1088/0264-9381/25/11/114033

Report number:

AEI-2007-169

View in:

ADS Abstract Service

reference search73 citations

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Abstract: (arXiv)

Coalescing binary black-hole systems are among the most promising sources of gravitational waves for ground-based interferometers. While the \emph{inspiral} and \emph{ring-down} stages of the binary black-hole coalescence are well-modelled by analytical approximation methods in general relativity, the recent progress in numerical relativity has enabled us to compute accurate waveforms from the \emph{merger} stage also. This has an important impact on the search for gravitational waves from binary black holes. In particular, while the current gravitational-wave searches look for each stage of the coalescence separately, combining the results from analytical and numerical relativity enables us to \emph{coherently} search for all three stages using a single template family. `Complete' binary black-hole waveforms can now be produced by matching post-Newtonian waveforms with those computed by numerical relativity. These waveforms can be parametrised to produce analytical waveform templates. The `complete' waveforms can also be used to estimate the efficiency of different search methods aiming to detect signals from black-hole coalescences. This paper summarises some recent efforts in this direction.

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