Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration
The Numerical-Relativity-Analytical-Relativity (NRAR) collaboration is a joint effort between members of the numerical relativity, analytical relativity and gravitational-wave data analysis communities. The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact bina...
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| creator | Hinder, Ian Buonanno, Alessandra Boyle, Michael Etienne, Zachariah B Healy, James Johnson-McDaniel, Nathan K Nagar, Alessandro Nakano, Hiroyuki Pan, Yi Pfeiffer, Harald P Pürrer, Michael Reisswig, Christian Scheel, Mark A Schnetter, Erik Sperhake, Ulrich Szilágyi, Bela Tichy, Wolfgang Wardell, Barry Zenginoglu, Anıl Alic, Daniela Bernuzzi, Sebastiano Bode, Tanja Brügmann, Bernd Buchman, Luisa T Campanelli, Manuela Chu, Tony Damour, Thibault Grigsby, Jason D Hannam, Mark Haas, Roland Hemberger, Daniel A Husa, Sascha Kidder, Lawrence E Laguna, Pablo London, Lionel Lovelace, Geoffrey Lousto, Carlos O Marronetti, Pedro Matzner, Richard A Mösta, Philipp Mroué, Abdul Müller, Doreen Mundim, Bruno C Nerozzi, Andrea Paschalidis, Vasileios Pollney, Denis Reifenberger, George Rezzolla, Luciano Shapiro, Stuart L Shoemaker, Deirdre Taracchini, Andrea Taylor, Nicholas W Teukolsky, Saul A Thierfelder, Marcus Witek, Helvi Zlochower, Yosef |
| description | The Numerical-Relativity-Analytical-Relativity (NRAR) collaboration is a joint effort between members of the numerical relativity, analytical relativity and gravitational-wave data analysis communities. The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact binaries and use them to develop accurate analytical templates for the LIGO/Virgo Collaboration to use in detecting gravitational-wave signals and extracting astrophysical information from them. We describe the results of the first stage of the NRAR project, which focused on producing an initial set of numerical waveforms from binary black holes with moderate mass ratios and spins, as well as one non-spinning binary configuration which has a mass ratio of 10. All of the numerical waveforms are analysed in a uniform and consistent manner, with numerical errors evaluated using an analysis code created by members of the NRAR collaboration. We compare previously-calibrated, non-precessing analytical waveforms, notably the effective-one-body (EOB) and phenomenological template families, to the newly-produced numerical waveforms. We find that when the binary's total mass is ~100-200 solar masses, current EOB and phenomenological models of spinning, non-precessing binary waveforms have overlaps above 99% (for advanced LIGO) with all of the non-precessing-binary numerical waveforms with mass ratios |
| doi_str_mv | 10.48550/arxiv.1307.5307 |
| format | Article |
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The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact binaries and use them to develop accurate analytical templates for the LIGO/Virgo Collaboration to use in detecting gravitational-wave signals and extracting astrophysical information from them. We describe the results of the first stage of the NRAR project, which focused on producing an initial set of numerical waveforms from binary black holes with moderate mass ratios and spins, as well as one non-spinning binary configuration which has a mass ratio of 10. All of the numerical waveforms are analysed in a uniform and consistent manner, with numerical errors evaluated using an analysis code created by members of the NRAR collaboration. We compare previously-calibrated, non-precessing analytical waveforms, notably the effective-one-body (EOB) and phenomenological template families, to the newly-produced numerical waveforms. We find that when the binary's total mass is ~100-200 solar masses, current EOB and phenomenological models of spinning, non-precessing binary waveforms have overlaps above 99% (for advanced LIGO) with all of the non-precessing-binary numerical waveforms with mass ratios <= 4, when maximizing over binary parameters. This implies that the loss of event rate due to modelling error is below 3%. Moreover, the non-spinning EOB waveforms previously calibrated to five non-spinning waveforms with mass ratio smaller than 6 have overlaps above 99.7% with the numerical waveform with a mass ratio of 10, without even maximizing on the binary parameters.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1307.5307</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Binary stars ; Black holes ; Collaboration ; Computer simulation ; Data analysis ; Error analysis ; Gravitation ; Gravitational waves ; Mass ratios ; Mathematical models ; Maximization ; Numerical relativity ; Optimization ; Parameters ; Physics - General Relativity and Quantum Cosmology ; Relativity ; Waveforms</subject><ispartof>arXiv.org, 2013-12</ispartof><rights>2013. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.1307.5307$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1088/0264-9381/31/2/025012$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Hinder, Ian</creatorcontrib><creatorcontrib>Buonanno, Alessandra</creatorcontrib><creatorcontrib>Boyle, Michael</creatorcontrib><creatorcontrib>Etienne, Zachariah B</creatorcontrib><creatorcontrib>Healy, James</creatorcontrib><creatorcontrib>Johnson-McDaniel, Nathan K</creatorcontrib><creatorcontrib>Nagar, Alessandro</creatorcontrib><creatorcontrib>Nakano, Hiroyuki</creatorcontrib><creatorcontrib>Pan, Yi</creatorcontrib><creatorcontrib>Pfeiffer, Harald P</creatorcontrib><creatorcontrib>Pürrer, Michael</creatorcontrib><creatorcontrib>Reisswig, Christian</creatorcontrib><creatorcontrib>Scheel, Mark A</creatorcontrib><creatorcontrib>Schnetter, Erik</creatorcontrib><creatorcontrib>Sperhake, Ulrich</creatorcontrib><creatorcontrib>Szilágyi, Bela</creatorcontrib><creatorcontrib>Tichy, Wolfgang</creatorcontrib><creatorcontrib>Wardell, Barry</creatorcontrib><creatorcontrib>Zenginoglu, Anıl</creatorcontrib><creatorcontrib>Alic, Daniela</creatorcontrib><creatorcontrib>Bernuzzi, Sebastiano</creatorcontrib><creatorcontrib>Bode, Tanja</creatorcontrib><creatorcontrib>Brügmann, Bernd</creatorcontrib><creatorcontrib>Buchman, Luisa T</creatorcontrib><creatorcontrib>Campanelli, Manuela</creatorcontrib><creatorcontrib>Chu, Tony</creatorcontrib><creatorcontrib>Damour, Thibault</creatorcontrib><creatorcontrib>Grigsby, Jason D</creatorcontrib><creatorcontrib>Hannam, Mark</creatorcontrib><creatorcontrib>Haas, Roland</creatorcontrib><creatorcontrib>Hemberger, Daniel A</creatorcontrib><creatorcontrib>Husa, Sascha</creatorcontrib><creatorcontrib>Kidder, Lawrence E</creatorcontrib><creatorcontrib>Laguna, Pablo</creatorcontrib><creatorcontrib>London, Lionel</creatorcontrib><creatorcontrib>Lovelace, Geoffrey</creatorcontrib><creatorcontrib>Lousto, Carlos O</creatorcontrib><creatorcontrib>Marronetti, Pedro</creatorcontrib><creatorcontrib>Matzner, Richard A</creatorcontrib><creatorcontrib>Mösta, Philipp</creatorcontrib><creatorcontrib>Mroué, Abdul</creatorcontrib><creatorcontrib>Müller, Doreen</creatorcontrib><creatorcontrib>Mundim, Bruno C</creatorcontrib><creatorcontrib>Nerozzi, Andrea</creatorcontrib><creatorcontrib>Paschalidis, Vasileios</creatorcontrib><creatorcontrib>Pollney, Denis</creatorcontrib><creatorcontrib>Reifenberger, George</creatorcontrib><creatorcontrib>Rezzolla, Luciano</creatorcontrib><creatorcontrib>Shapiro, Stuart L</creatorcontrib><creatorcontrib>Shoemaker, Deirdre</creatorcontrib><creatorcontrib>Taracchini, Andrea</creatorcontrib><creatorcontrib>Taylor, Nicholas W</creatorcontrib><creatorcontrib>Teukolsky, Saul A</creatorcontrib><creatorcontrib>Thierfelder, Marcus</creatorcontrib><creatorcontrib>Witek, Helvi</creatorcontrib><creatorcontrib>Zlochower, Yosef</creatorcontrib><title>Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration</title><title>arXiv.org</title><description>The Numerical-Relativity-Analytical-Relativity (NRAR) collaboration is a joint effort between members of the numerical relativity, analytical relativity and gravitational-wave data analysis communities. The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact binaries and use them to develop accurate analytical templates for the LIGO/Virgo Collaboration to use in detecting gravitational-wave signals and extracting astrophysical information from them. We describe the results of the first stage of the NRAR project, which focused on producing an initial set of numerical waveforms from binary black holes with moderate mass ratios and spins, as well as one non-spinning binary configuration which has a mass ratio of 10. All of the numerical waveforms are analysed in a uniform and consistent manner, with numerical errors evaluated using an analysis code created by members of the NRAR collaboration. We compare previously-calibrated, non-precessing analytical waveforms, notably the effective-one-body (EOB) and phenomenological template families, to the newly-produced numerical waveforms. We find that when the binary's total mass is ~100-200 solar masses, current EOB and phenomenological models of spinning, non-precessing binary waveforms have overlaps above 99% (for advanced LIGO) with all of the non-precessing-binary numerical waveforms with mass ratios <= 4, when maximizing over binary parameters. This implies that the loss of event rate due to modelling error is below 3%. Moreover, the non-spinning EOB waveforms previously calibrated to five non-spinning waveforms with mass ratio smaller than 6 have overlaps above 99.7% with the numerical waveform with a mass ratio of 10, without even maximizing on the binary parameters.</description><subject>Binary stars</subject><subject>Black holes</subject><subject>Collaboration</subject><subject>Computer simulation</subject><subject>Data analysis</subject><subject>Error analysis</subject><subject>Gravitation</subject><subject>Gravitational waves</subject><subject>Mass ratios</subject><subject>Mathematical models</subject><subject>Maximization</subject><subject>Numerical relativity</subject><subject>Optimization</subject><subject>Parameters</subject><subject>Physics - General Relativity and Quantum Cosmology</subject><subject>Relativity</subject><subject>Waveforms</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotkEtrwzAQhEWh0JDm3lMR9Ox0JVm2fAwhfUBoIeRu1pZEHWQrley0-fd1nF52YWdYZj5CHhgsUyUlPGP4bU5LJiBfynHckBkXgiUq5fyOLGI8AADPci6lmBG3CcGHBDt059hEip2mtW-PGJroO9p7Okl9U6OjrdfGReot7YbWhOn2gydjfWgjPQavh9poWp1p_2Xox261o2vvHFY-YN_47p7cWnTRLP73nOxfNvv1W7L9fH1fr7YJSlYkhRW6sBy1FRbGnLllPBN5nSPoDEcFCqXSLM0MgkFpmUArgXOomcpVVYs5eby-nUiUx9C0GM7lhUh5ITIanq6GMfL3YGJfHvwQxp6x5KBkISSIQvwBZiRk0A</recordid><startdate>20131211</startdate><enddate>20131211</enddate><creator>Hinder, Ian</creator><creator>Buonanno, Alessandra</creator><creator>Boyle, Michael</creator><creator>Etienne, Zachariah B</creator><creator>Healy, James</creator><creator>Johnson-McDaniel, Nathan K</creator><creator>Nagar, Alessandro</creator><creator>Nakano, Hiroyuki</creator><creator>Pan, Yi</creator><creator>Pfeiffer, Harald P</creator><creator>Pürrer, Michael</creator><creator>Reisswig, Christian</creator><creator>Scheel, Mark A</creator><creator>Schnetter, Erik</creator><creator>Sperhake, Ulrich</creator><creator>Szilágyi, Bela</creator><creator>Tichy, Wolfgang</creator><creator>Wardell, Barry</creator><creator>Zenginoglu, Anıl</creator><creator>Alic, Daniela</creator><creator>Bernuzzi, Sebastiano</creator><creator>Bode, Tanja</creator><creator>Brügmann, Bernd</creator><creator>Buchman, Luisa T</creator><creator>Campanelli, Manuela</creator><creator>Chu, Tony</creator><creator>Damour, Thibault</creator><creator>Grigsby, Jason D</creator><creator>Hannam, Mark</creator><creator>Haas, Roland</creator><creator>Hemberger, Daniel A</creator><creator>Husa, Sascha</creator><creator>Kidder, Lawrence E</creator><creator>Laguna, Pablo</creator><creator>London, Lionel</creator><creator>Lovelace, Geoffrey</creator><creator>Lousto, Carlos O</creator><creator>Marronetti, Pedro</creator><creator>Matzner, Richard A</creator><creator>Mösta, Philipp</creator><creator>Mroué, Abdul</creator><creator>Müller, Doreen</creator><creator>Mundim, Bruno C</creator><creator>Nerozzi, Andrea</creator><creator>Paschalidis, Vasileios</creator><creator>Pollney, Denis</creator><creator>Reifenberger, George</creator><creator>Rezzolla, Luciano</creator><creator>Shapiro, Stuart L</creator><creator>Shoemaker, Deirdre</creator><creator>Taracchini, Andrea</creator><creator>Taylor, Nicholas W</creator><creator>Teukolsky, Saul A</creator><creator>Thierfelder, Marcus</creator><creator>Witek, Helvi</creator><creator>Zlochower, Yosef</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20131211</creationdate><title>Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration</title><author>Hinder, Ian ; Buonanno, Alessandra ; Boyle, Michael ; Etienne, Zachariah B ; Healy, James ; Johnson-McDaniel, Nathan K ; Nagar, Alessandro ; Nakano, Hiroyuki ; Pan, Yi ; Pfeiffer, Harald P ; Pürrer, Michael ; Reisswig, Christian ; Scheel, Mark A ; Schnetter, Erik ; Sperhake, Ulrich ; Szilágyi, Bela ; Tichy, Wolfgang ; Wardell, Barry ; Zenginoglu, Anıl ; Alic, Daniela ; Bernuzzi, Sebastiano ; Bode, Tanja ; Brügmann, Bernd ; Buchman, Luisa T ; Campanelli, Manuela ; Chu, Tony ; Damour, Thibault ; Grigsby, Jason D ; Hannam, Mark ; Haas, Roland ; Hemberger, Daniel A ; Husa, Sascha ; Kidder, Lawrence E ; Laguna, Pablo ; London, Lionel ; Lovelace, Geoffrey ; Lousto, Carlos O ; Marronetti, Pedro ; Matzner, Richard A ; Mösta, Philipp ; Mroué, Abdul ; Müller, Doreen ; Mundim, Bruno C ; Nerozzi, Andrea ; Paschalidis, Vasileios ; Pollney, Denis ; Reifenberger, George ; Rezzolla, Luciano ; Shapiro, Stuart L ; Shoemaker, Deirdre ; Taracchini, Andrea ; Taylor, Nicholas W ; Teukolsky, Saul A ; Thierfelder, Marcus ; Witek, Helvi ; Zlochower, Yosef</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a519-9f3d9f2adf3f06727f12637c7a0d6a9f209884646ea0ea5f13af50220c1878bc3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>Binary stars</topic><topic>Black 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Anıl</au><au>Alic, Daniela</au><au>Bernuzzi, Sebastiano</au><au>Bode, Tanja</au><au>Brügmann, Bernd</au><au>Buchman, Luisa T</au><au>Campanelli, Manuela</au><au>Chu, Tony</au><au>Damour, Thibault</au><au>Grigsby, Jason D</au><au>Hannam, Mark</au><au>Haas, Roland</au><au>Hemberger, Daniel A</au><au>Husa, Sascha</au><au>Kidder, Lawrence E</au><au>Laguna, Pablo</au><au>London, Lionel</au><au>Lovelace, Geoffrey</au><au>Lousto, Carlos O</au><au>Marronetti, Pedro</au><au>Matzner, Richard A</au><au>Mösta, Philipp</au><au>Mroué, Abdul</au><au>Müller, Doreen</au><au>Mundim, Bruno C</au><au>Nerozzi, Andrea</au><au>Paschalidis, Vasileios</au><au>Pollney, Denis</au><au>Reifenberger, George</au><au>Rezzolla, Luciano</au><au>Shapiro, Stuart L</au><au>Shoemaker, Deirdre</au><au>Taracchini, Andrea</au><au>Taylor, Nicholas W</au><au>Teukolsky, Saul A</au><au>Thierfelder, Marcus</au><au>Witek, Helvi</au><au>Zlochower, Yosef</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration</atitle><jtitle>arXiv.org</jtitle><date>2013-12-11</date><risdate>2013</risdate><eissn>2331-8422</eissn><abstract>The Numerical-Relativity-Analytical-Relativity (NRAR) collaboration is a joint effort between members of the numerical relativity, analytical relativity and gravitational-wave data analysis communities. The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact binaries and use them to develop accurate analytical templates for the LIGO/Virgo Collaboration to use in detecting gravitational-wave signals and extracting astrophysical information from them. We describe the results of the first stage of the NRAR project, which focused on producing an initial set of numerical waveforms from binary black holes with moderate mass ratios and spins, as well as one non-spinning binary configuration which has a mass ratio of 10. All of the numerical waveforms are analysed in a uniform and consistent manner, with numerical errors evaluated using an analysis code created by members of the NRAR collaboration. We compare previously-calibrated, non-precessing analytical waveforms, notably the effective-one-body (EOB) and phenomenological template families, to the newly-produced numerical waveforms. We find that when the binary's total mass is ~100-200 solar masses, current EOB and phenomenological models of spinning, non-precessing binary waveforms have overlaps above 99% (for advanced LIGO) with all of the non-precessing-binary numerical waveforms with mass ratios <= 4, when maximizing over binary parameters. This implies that the loss of event rate due to modelling error is below 3%. Moreover, the non-spinning EOB waveforms previously calibrated to five non-spinning waveforms with mass ratio smaller than 6 have overlaps above 99.7% with the numerical waveform with a mass ratio of 10, without even maximizing on the binary parameters.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1307.5307</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2013-12 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_1307_5307 |
| source | arXiv.org; Free E- Journals |
| subjects | Binary stars Black holes Collaboration Computer simulation Data analysis Error analysis Gravitation Gravitational waves Mass ratios Mathematical models Maximization Numerical relativity Optimization Parameters Physics - General Relativity and Quantum Cosmology Relativity Waveforms |
| title | Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration |
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