Phenomenological template family for black-hole coalescence waveforms

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dc.creatorAjith, P.
dc.creatorBabak, S.
dc.creatorChen, Y.
dc.creatorHewitson, M.
dc.creatorKrishnan, B.
dc.creatorWhelan, J. T.
dc.creatorBruegmann, B.
dc.creatorDiener, P.
dc.creatorGonzalez, J.
dc.creatorHannam, M.
dc.creatorHusa, S.
dc.creatorKoppitz, M.
dc.creatorPollney, D.
dc.creatorRezzolla, L.
dc.creatorSantamaria, L.
dc.creatorSintes, A. M.
dc.creatorSperhake, U.
dc.creatorThornburg, J.
dc.date2007-04-30
dc.date2007-07-11
dc.date.accessioned2026-07-07T11:56:45Z
dc.date.available2026-07-07T11:56:45Z
dc.descriptionRecent progress in numerical relativity has enabled us to model the non-perturbative merger phase of the binary black-hole coalescence problem. Based on these results, we propose a phenomenological family of waveforms which can model the inspiral, merger, and ring-down stages of black hole coalescence. We also construct a template bank using this family of waveforms and discuss its implementation in the search for signatures of gravitational waves produced by black-hole coalescences in the data of ground-based interferometers. This template bank might enable us to extend the present inspiral searches to higher-mass binary black-hole systems, i.e., systems with total mass greater than about 80 solar masses, thereby increasing the reach of the current generation of ground-based detectors.
dc.descriptionMinor changes, Submitted to Class. Quantum Grav. (Proc. GWDAW11)
dc.identifierhttps://arxiv.org/abs/0704.3764
dc.identifierhttp://arxiv.org/abs/0704.3764
dc.identifierClass.Quant.Grav.24:S689-S700,2007
dc.identifierdoi:10.1088/0264-9381/24/19/S31
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205640
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.titlePhenomenological template family for black-hole coalescence waveforms
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