A phenomenological template family for black-hole coalescence waveforms

Ajith, P.; Babak, S.; Chen, Y.; Hewitson, M.; Krishnan, B.; Whelan, J. T.; Brügmann, Bernd; Diener, Peter; González, José Antonio García-Cruces; Hannam, M. D.; Husa, S.; Koppitz, Michael; Pollney, Denis; Rezzolla, Luciano; Santamaría, L.; Sintes, A. M.; Sperhake, Ulrich; Thornburg, Jonathan

doi:10.1088/0264-9381/24/19/s31

Cited by 288 publications

(320 citation statements)

References 35 publications

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“…6.9 we show the agreement between state-of-the-art EOB [279] and NR waveforms for an equal-mass BH-BH binary with both spins aligned with the orbital-angular momentum and quasi-extremal (top panel), and a single-spin binary BH with mass ratio 5, precessing with mild spin magnitude (bottom panel). Starting with [345,357], a more phenomenological avenue has also been followed to produce inspiral-merger-ringdown waveforms. In this case, the original motivation was to provide aLIGO/AdV detectors with inspiral, merger and ringdown waveforms that could be computed efficiently during searches and be used to detect high-mass coalescing compact binaries.…”

Section: Interface Between Theory and Observationsmentioning

confidence: 99%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

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Section: Interface Between Theory and Observationsmentioning

confidence: 99%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

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“…As the total mass of the system increases, the analytical PN inspiral waveforms become inadequate because only the merger and ringdown waves have significant power in the sensitive band of the detectors. For this reason, this search (and a template search for binary black holes with the total mass between 25 and 100 M [18]) uses the full IMR waveforms from two different families: the Effective One Body Numerical Relativity (EOBNR) family [9,10,12,51] and the IMRPhenom family [11,52,53]. The EOBNR waveform family uses the Effective One Body (EOB) Hamiltonian to evolve the binary system up to the merger.…”

Section: Simulationsmentioning

confidence: 99%

Search for gravitational waves from intermediate mass binary black holes

Abadie¹,

Abbott²,

Abbott³

et al. 2012

Phys. Rev. D

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We present the results of a weakly modeled burst search for gravitational waves from mergers of non-spinning intermediate mass black holes (IMBH) in the total mass range 100-450 M and with the component mass ratios between 1:1 and 4:1. The search was conducted on data collected by the LIGO and Virgo detectors between November of 2005 and October of 2007. No plausible signals were observed by the search which constrains the astrophysical rates of the IMBH mergers as a function of the component masses. In the most efficiently detected bin centered on 88 + 88 M , for non-spinning sources, the rate density upper limit is 0.13 per Mpc 3 per Myr at the 90% confidence level.

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“…These systems generate well understood "chirp" gravitational-wave signals, which have been computed using post-Newtonian approximation [13,14] or numerical relativity simulations [15]. One can then search for the chirp signals using matched template techniques -indeed a number of such searches have been performed using LIGO and Virgo data [16][17][18].…”

Section: Introductionmentioning

confidence: 99%

Accessibility of the gravitational-wave background due to binary coalescences to second and third generation gravitational-wave detectors

2012

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International audienceCompact binary coalescences, such as binary neutron stars or black holes, are among the most promising candidate sources for the current and future terrestrial gravitational-wave detectors. While such sources are best searched using matched template techniques and chirp template banks, integrating chirp signals from binaries over the entire universe also leads to a gravitational-wave background (GWB). In this paper we systematically scan the parameter space for the binary coalescence GWB models, taking into account uncertainties in the star formation rate and in the delay time between the formation and coalescence of the binary, and we compare the computed GWB to the expected sensitivities of the second and third generation gravitational-wave detector networks. We find that second generation detectors are likely to detect the binary coalescence GWB, while the third generation detectors will probe most of the available parameter space. The binary coalescence GWB will, in fact, be a foreground for the third generation detectors, potentially masking the GWB background due to cosmological sources. Accessing the cosmological GWB with third generation detectors will therefore require identification and subtraction of all inspiral signals from all binaries in the detectors’ frequency band

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A phenomenological template family for black-hole coalescence waveforms

Cited by 288 publications

References 35 publications

Sources of Gravitational Waves: Theory and Observations

Sources of Gravitational Waves: Theory and Observations

Search for gravitational waves from intermediate mass binary black holes

Accessibility of the gravitational-wave background due to binary coalescences to second and third generation gravitational-wave detectors

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