CaltechAUTHORS
  A Caltech Library Service

Length requirements for numerical-relativity waveforms

Hannam, Mark and Husa, Sascha and Ohme, Frank and Ajith, P. (2010) Length requirements for numerical-relativity waveforms. Physical Review D, 82 (12). Art. No. 124052. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20110314-113342584

[img]
Preview
PDF - Published Version
See Usage Policy.

486Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20110314-113342584

Abstract

One way to produce complete inspiral-merger-ringdown gravitational waveforms from black-hole-binary systems is to connect post-Newtonian (PN) and numerical-relativity (NR) results to create “hybrid” waveforms. Hybrid waveforms are central to the construction of some phenomenological models for gravitational-wave (GW) search templates, and for tests of GW search pipelines. The dominant error source in hybrid waveforms arises from the PN contribution, and can be reduced by increasing the number of NR GW cycles that are included in the hybrid. Hybrid waveforms are considered sufficiently accurate for GW detection if their mismatch error is below 3% (i.e., a fitting factor above 0.97). We address the question of the length requirements of NR waveforms such that the final hybrid waveforms meet this requirement, considering nonspinning binaries with q=M_2/M_1 ∈ [1,4] and equal-mass binaries with χ=Si/Mi_2 ∈ [-0.5,0.5]. We conclude that, for the cases we study, simulations must contain between three (in the equal-mass nonspinning case) and ten (the χ=0.5 case) orbits before merger, but there is also evidence that these are the regions of parameter space for which the least number of cycles will be needed.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1103/PhysRevD.82.124052DOIUNSPECIFIED
http://link.aps.org/doi/10.1103/PhysRevD.82.124052PublisherUNSPECIFIED
ORCID:
AuthorORCID
Ajith, P.0000-0001-7519-2439
Additional Information:© 2010 American Physical Society. Received 16 September 2010; published 22 December 2010. We thank Steve Fairhurst and Harald Pfeiffer for useful discussions, and Sukanta Bose and Doreen Müller for helpful comments on the manuscript. M. Hannam was supported by an FWF Lise-Meitner Fellowship (M1178- N16) and a Science and Technology Facilities Council Advanced Fellowship (ST/H008438/1). S. Husa was supported by Grant No. FPA-2007-60220 from the Spanish Ministry of Science, the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, and DAAD Grant No. D/07/13385. F. Ohme thanks the IMPRS for Gravitational Wave Astronomy and the DLR (Deutsches Zentrum für Luftund Raumfahrt) for support. P. A. was supported in part by NSF Grants No. PHY-0653653 and No. PHY-0601459, and the David and Barbara Groce Fund at Caltech. BAM simulations were carried out at LRZ Munich, ICHEC Dublin, the Vienna Scientific Cluster (VSC), at MareNostrum at Barcelona Supercomputing Center—Centro Nacional de Supercomputación (Spanish National Supercomputing Center), and CESGA, Santiago the Compostela.
Group:TAPIR
Funders:
Funding AgencyGrant Number
FWF Lise-Meitner FellowshipM1178- N16
Science and Technology Facilities Council Advanced FellowshipST/H008438/1
Spanish Ministry of ScienceFPA-2007-60220
Spanish MICINNsCSD2009-00064
Deutscher Akademischer Austausch Dienst (DAAD)D/07/13385
IMPRS for Gravitational Wave AstronomyUNSPECIFIED
Deutsches Zentrum fur Luftund Raumfahrt (DLR)UNSPECIFIED
NSFPHY-0653653
NSFPHY-0601459
Issue or Number:12
Classification Code:PACS: 04.30.Db, 04.25.D-, 04.25.Nx
Record Number:CaltechAUTHORS:20110314-113342584
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110314-113342584
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:22860
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:15 Mar 2011 14:58
Last Modified:09 Mar 2020 13:18

Repository Staff Only: item control page