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Effective-one-body waveforms for binary neutron stars using surrogate models

Lackey, Benjamin D. and Bernuzzi, Sebastiano and Galley, Chad R. and Meidam, Jeroen and Van Den Broeck, Chris (2017) Effective-one-body waveforms for binary neutron stars using surrogate models. Physical Review D, 95 (10). Art. No. 104036. ISSN 2470-0010. doi:10.1103/PhysRevD.95.104036.

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Gravitational-wave observations of binary neutron star systems can provide information about the masses, spins, and structure of neutron stars. However, this requires accurate and computationally efficient waveform models that take ≲1  s to evaluate for use in Bayesian parameter estimation codes that perform 10^7–10^8 waveform evaluations. We present a surrogate model of a nonspinning effective-one-body waveform model with ℓ=2 , 3, and 4 tidal multipole moments that reproduces waveforms of binary neutron star numerical simulations up to merger. The surrogate is built from compact sets of effective-one-body waveform amplitude and phase data that each form a reduced basis. We find that 12 amplitude and 7 phase basis elements are sufficient to reconstruct any binary neutron star waveform with a starting frequency of 10 Hz. The surrogate has maximum errors of 3.8% in amplitude (0.04% excluding the last 100M before merger) and 0.043 rad in phase. This leads to typical mismatches of 10^(−5)−10^(−4) for Advanced LIGO depending on the component masses, with a worst case match of 7×10^(−4) when both stars have masses ≥2  M⊙ . The version implemented in the LIGO Algorithm Library takes ∼0.07  s to evaluate for a starting frequency of 30 Hz and ∼0.8  s for a starting frequency of 10 Hz, resulting in a speed-up factor of O(10^3) relative to the original MATLAB code. This allows parameter estimation codes to run in days to weeks rather than years, and we demonstrate this with a nested sampling run that recovers the masses and tidal parameters of a simulated binary neutron star system.

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Additional Information:© 2017 American Physical Society. Received 15 October 2016; published 30 May 2017. B. L. thanks Larne Pekowsky and Duncan Brown for significant computing help and Rory Smith and Michael Pürrer for helpful discussions at the beginning of this work. S. B. thanks Paolo Pani for helpful discussions about Λ3,4fit(Λ2) fits. B. L. was supported by National Science Foundation (NSF) Grant No. AST-1333142. S. B. was supported by a Rita Levi Montalcini fellowship of the Italian Ministry of Education, University and Research (MIUR). C. R. G was supported in part by NSF Grant No. PHY-1404569 to Caltech and by the Sherman Fairchild Foundation. J. M. and C. V. D. B. were supported by the research program of the Foundation for Fundamental Research on Matter (FOM), which is partially supported by the Netherlands Organisation for Scientific Research (NWO). Computations were performed on the Syracuse University Campus Grid which is supported by NSF Grants No. ACI-1341006 and No. ACI-1541396, and by Syracuse University ITS.
Group:Walter Burke Institute for Theoretical Physics
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Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Stichting voor Fundamenteel Onderzoek der Materie (FOM)UNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
Syracuse UniversityUNSPECIFIED
Issue or Number:10
Record Number:CaltechAUTHORS:20170531-094625131
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:77849
Deposited By: Tony Diaz
Deposited On:31 May 2017 17:00
Last Modified:15 Nov 2021 17:34

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