First all-sky search for continuous gravitational waves from unknown sources in binary systems
We present the first results of an all-sky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO Science R...
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| creator | The LIGO Scientific Collaboration Acernese, F Agathos, M Allocca, A Anderson, R Bartos, I Bloemen, S Born, M Boschi, V Brau, J E Bridges, D O Buonanno, A Cao, J Chamberlin, S J Christensen, N Conte, A Corpuz, A J -P Coulon Countryman, S Dayanga, T DeSalvo, R Donath, A Downes, T P Drago, M Effler, A Eggenstein, H Fejer, M M Feroz, F Fisher, R P Frasca, S Fulda, P Goetz, E Gräf, C Groot, P Grover, K Hammer, D Hanke, M Hartman, M T C -J Haster Heitmann, H Hooper, S Hosken, D J Huynh-Dinh, T Ivanov, A James, E Y Ji Jones, R Kalogera, V Karlen, J Kawazoe, F Kim, N G Kuo, L Kutynia, A C -H Lee Luijten, E Macdonald, E P Malvezzi, V Mandic, V Mangano, V Martin, R M Mazumder, N McCarthy, R McIver, J Melatos, A Moesta, P Nitz, A Ochsner, E Oppermann, P Pedraza, M Phelps, M Prasad, J Prix, R Prodi, G A Puncken, O Puppo, P Rabeling, D S Rácz, I Regimbau, T Riles, K Robinet, F Rocchi, A Rüdiger, A Schuette, D Shaddock, D Singh, R Smith, M Stops, D Tomlinson, C Ugolini, D Vajente, G Vaulin, R Verma, S S Wade, M Wessels, P Wette, K Wiesner, K Williams, K Williams, T Winkler, W Zucker, M E |
| description | We present the first results of an all-sky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO Science Run and the second and third Virgo Science Runs. The search covers a range of frequencies from 20 Hz to 520 Hz, a range of orbital periods from 2 to ~2,254 h and a frequency- and period-dependent range of frequency modulation depths from 0.277 to 100 mHz. This corresponds to a range of projected semi-major axes of the orbit from ~0.6e-3 ls to ~6,500 ls assuming the orbit of the binary is circular. While no plausible candidate gravitational wave events survive the pipeline, upper limits are set on the analyzed data. The most sensitive 95% confidence upper limit obtained on gravitational wave strain is 2.3e-24 at 217 Hz, assuming the source waves are circularly polarized. Although this search has been optimized for circular binary orbits, the upper limits obtained remain valid for orbital eccentricities as large as 0.9. In addition, upper limits are placed on continuous gravitational wave emission from the low-mass x-ray binary Scorpius X-1 between 20 Hz and 57.25 Hz. |
| doi_str_mv | 10.48550/arxiv.1405.7904 |
| format | Article |
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Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO Science Run and the second and third Virgo Science Runs. The search covers a range of frequencies from 20 Hz to 520 Hz, a range of orbital periods from 2 to ~2,254 h and a frequency- and period-dependent range of frequency modulation depths from 0.277 to 100 mHz. This corresponds to a range of projected semi-major axes of the orbit from ~0.6e-3 ls to ~6,500 ls assuming the orbit of the binary is circular. While no plausible candidate gravitational wave events survive the pipeline, upper limits are set on the analyzed data. The most sensitive 95% confidence upper limit obtained on gravitational wave strain is 2.3e-24 at 217 Hz, assuming the source waves are circularly polarized. Although this search has been optimized for circular binary orbits, the upper limits obtained remain valid for orbital eccentricities as large as 0.9. In addition, upper limits are placed on continuous gravitational wave emission from the low-mass x-ray binary Scorpius X-1 between 20 Hz and 57.25 Hz.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1405.7904</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Algorithms ; Binary stars ; Circular polarization ; Eccentric orbits ; Frequency modulation ; Gravitation ; Gravitational waves ; Neutron stars ; Physics - General Relativity and Quantum Cosmology ; Physics - High Energy Astrophysical Phenomena ; Searching ; X ray binaries ; X ray stars</subject><ispartof>arXiv.org, 2014-09</ispartof><rights>2014. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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K</creatorcontrib><creatorcontrib>Williams, T</creatorcontrib><creatorcontrib>Winkler, W</creatorcontrib><creatorcontrib>Zucker, M E</creatorcontrib><title>First all-sky search for continuous gravitational waves from unknown sources in binary systems</title><title>arXiv.org</title><description>We present the first results of an all-sky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO Science Run and the second and third Virgo Science Runs. The search covers a range of frequencies from 20 Hz to 520 Hz, a range of orbital periods from 2 to ~2,254 h and a frequency- and period-dependent range of frequency modulation depths from 0.277 to 100 mHz. This corresponds to a range of projected semi-major axes of the orbit from ~0.6e-3 ls to ~6,500 ls assuming the orbit of the binary is circular. While no plausible candidate gravitational wave events survive the pipeline, upper limits are set on the analyzed data. The most sensitive 95% confidence upper limit obtained on gravitational wave strain is 2.3e-24 at 217 Hz, assuming the source waves are circularly polarized. Although this search has been optimized for circular binary orbits, the upper limits obtained remain valid for orbital eccentricities as large as 0.9. In addition, upper limits are placed on continuous gravitational wave emission from the low-mass x-ray binary Scorpius X-1 between 20 Hz and 57.25 Hz.</description><subject>Algorithms</subject><subject>Binary stars</subject><subject>Circular polarization</subject><subject>Eccentric orbits</subject><subject>Frequency modulation</subject><subject>Gravitation</subject><subject>Gravitational waves</subject><subject>Neutron stars</subject><subject>Physics - General Relativity and Quantum Cosmology</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Searching</subject><subject>X ray binaries</subject><subject>X ray 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P ; Goetz, E ; Gräf, C ; Groot, P ; Grover, K ; Hammer, D ; Hanke, M ; Hartman, M T ; C -J Haster ; Heitmann, H ; Hooper, S ; Hosken, D J ; Huynh-Dinh, T ; Ivanov, A ; James, E ; Y Ji ; Jones, R ; Kalogera, V ; Karlen, J ; Kawazoe, F ; Kim, N G ; Kuo, L ; Kutynia, A ; C -H Lee ; Luijten, E ; Macdonald, E P ; Malvezzi, V ; Mandic, V ; Mangano, V ; Martin, R M ; Mazumder, N ; McCarthy, R ; McIver, J ; Melatos, A ; Moesta, P ; Nitz, A ; Ochsner, E ; Oppermann, P ; Pedraza, M ; Phelps, M ; Prasad, J ; Prix, R ; Prodi, G A ; Puncken, O ; Puppo, P ; Rabeling, D S ; Rácz, I ; Regimbau, T ; Riles, K ; Robinet, F ; Rocchi, A ; Rüdiger, A ; Schuette, D ; Shaddock, D ; Singh, R ; Smith, M ; Stops, D ; Tomlinson, C ; Ugolini, D ; Vajente, G ; Vaulin, R ; Verma, S S ; Wade, M ; Wessels, P ; Wette, K ; Wiesner, K ; Williams, K ; Williams, T ; Winkler, W ; Zucker, M E</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a519-9206fbd0b7d37c2b7c03e138254ec8881047e7cec0ca14858134e74be99b0f543</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Algorithms</topic><topic>Binary stars</topic><topic>Circular polarization</topic><topic>Eccentric orbits</topic><topic>Frequency modulation</topic><topic>Gravitation</topic><topic>Gravitational waves</topic><topic>Neutron stars</topic><topic>Physics - General Relativity and Quantum Cosmology</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Searching</topic><topic>X ray binaries</topic><topic>X ray stars</topic><toplevel>online_resources</toplevel><creatorcontrib>The LIGO Scientific Collaboration</creatorcontrib><creatorcontrib>Acernese, F</creatorcontrib><creatorcontrib>Agathos, M</creatorcontrib><creatorcontrib>Allocca, A</creatorcontrib><creatorcontrib>Anderson, 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F</creatorcontrib><creatorcontrib>Fisher, R P</creatorcontrib><creatorcontrib>Frasca, S</creatorcontrib><creatorcontrib>Fulda, P</creatorcontrib><creatorcontrib>Goetz, E</creatorcontrib><creatorcontrib>Gräf, C</creatorcontrib><creatorcontrib>Groot, P</creatorcontrib><creatorcontrib>Grover, K</creatorcontrib><creatorcontrib>Hammer, D</creatorcontrib><creatorcontrib>Hanke, M</creatorcontrib><creatorcontrib>Hartman, M T</creatorcontrib><creatorcontrib>C -J Haster</creatorcontrib><creatorcontrib>Heitmann, H</creatorcontrib><creatorcontrib>Hooper, S</creatorcontrib><creatorcontrib>Hosken, D J</creatorcontrib><creatorcontrib>Huynh-Dinh, T</creatorcontrib><creatorcontrib>Ivanov, A</creatorcontrib><creatorcontrib>James, E</creatorcontrib><creatorcontrib>Y Ji</creatorcontrib><creatorcontrib>Jones, R</creatorcontrib><creatorcontrib>Kalogera, V</creatorcontrib><creatorcontrib>Karlen, J</creatorcontrib><creatorcontrib>Kawazoe, F</creatorcontrib><creatorcontrib>Kim, N G</creatorcontrib><creatorcontrib>Kuo, L</creatorcontrib><creatorcontrib>Kutynia, A</creatorcontrib><creatorcontrib>C -H Lee</creatorcontrib><creatorcontrib>Luijten, E</creatorcontrib><creatorcontrib>Macdonald, E P</creatorcontrib><creatorcontrib>Malvezzi, V</creatorcontrib><creatorcontrib>Mandic, V</creatorcontrib><creatorcontrib>Mangano, V</creatorcontrib><creatorcontrib>Martin, R M</creatorcontrib><creatorcontrib>Mazumder, N</creatorcontrib><creatorcontrib>McCarthy, R</creatorcontrib><creatorcontrib>McIver, J</creatorcontrib><creatorcontrib>Melatos, A</creatorcontrib><creatorcontrib>Moesta, P</creatorcontrib><creatorcontrib>Nitz, A</creatorcontrib><creatorcontrib>Ochsner, E</creatorcontrib><creatorcontrib>Oppermann, P</creatorcontrib><creatorcontrib>Pedraza, M</creatorcontrib><creatorcontrib>Phelps, M</creatorcontrib><creatorcontrib>Prasad, J</creatorcontrib><creatorcontrib>Prix, R</creatorcontrib><creatorcontrib>Prodi, G A</creatorcontrib><creatorcontrib>Puncken, O</creatorcontrib><creatorcontrib>Puppo, P</creatorcontrib><creatorcontrib>Rabeling, D S</creatorcontrib><creatorcontrib>Rácz, I</creatorcontrib><creatorcontrib>Regimbau, T</creatorcontrib><creatorcontrib>Riles, K</creatorcontrib><creatorcontrib>Robinet, F</creatorcontrib><creatorcontrib>Rocchi, A</creatorcontrib><creatorcontrib>Rüdiger, A</creatorcontrib><creatorcontrib>Schuette, D</creatorcontrib><creatorcontrib>Shaddock, D</creatorcontrib><creatorcontrib>Singh, R</creatorcontrib><creatorcontrib>Smith, M</creatorcontrib><creatorcontrib>Stops, D</creatorcontrib><creatorcontrib>Tomlinson, C</creatorcontrib><creatorcontrib>Ugolini, D</creatorcontrib><creatorcontrib>Vajente, G</creatorcontrib><creatorcontrib>Vaulin, R</creatorcontrib><creatorcontrib>Verma, S S</creatorcontrib><creatorcontrib>Wade, M</creatorcontrib><creatorcontrib>Wessels, P</creatorcontrib><creatorcontrib>Wette, K</creatorcontrib><creatorcontrib>Wiesner, K</creatorcontrib><creatorcontrib>Williams, K</creatorcontrib><creatorcontrib>Williams, T</creatorcontrib><creatorcontrib>Winkler, W</creatorcontrib><creatorcontrib>Zucker, M E</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>The LIGO Scientific Collaboration</au><au>Acernese, F</au><au>Agathos, M</au><au>Allocca, A</au><au>Anderson, R</au><au>Bartos, I</au><au>Bloemen, S</au><au>Born, M</au><au>Boschi, V</au><au>Brau, J E</au><au>Bridges, D O</au><au>Buonanno, A</au><au>Cao, J</au><au>Chamberlin, S J</au><au>Christensen, N</au><au>Conte, A</au><au>Corpuz, A</au><au>J -P Coulon</au><au>Countryman, S</au><au>Dayanga, T</au><au>DeSalvo, R</au><au>Donath, A</au><au>Downes, T P</au><au>Drago, M</au><au>Effler, A</au><au>Eggenstein, H</au><au>Fejer, M M</au><au>Feroz, F</au><au>Fisher, R P</au><au>Frasca, S</au><au>Fulda, P</au><au>Goetz, E</au><au>Gräf, C</au><au>Groot, P</au><au>Grover, K</au><au>Hammer, D</au><au>Hanke, M</au><au>Hartman, M T</au><au>C -J Haster</au><au>Heitmann, H</au><au>Hooper, S</au><au>Hosken, D J</au><au>Huynh-Dinh, T</au><au>Ivanov, A</au><au>James, E</au><au>Y Ji</au><au>Jones, R</au><au>Kalogera, V</au><au>Karlen, J</au><au>Kawazoe, F</au><au>Kim, N G</au><au>Kuo, L</au><au>Kutynia, A</au><au>C -H Lee</au><au>Luijten, E</au><au>Macdonald, E P</au><au>Malvezzi, V</au><au>Mandic, V</au><au>Mangano, V</au><au>Martin, R M</au><au>Mazumder, N</au><au>McCarthy, R</au><au>McIver, J</au><au>Melatos, A</au><au>Moesta, P</au><au>Nitz, A</au><au>Ochsner, E</au><au>Oppermann, P</au><au>Pedraza, M</au><au>Phelps, M</au><au>Prasad, J</au><au>Prix, R</au><au>Prodi, G A</au><au>Puncken, O</au><au>Puppo, P</au><au>Rabeling, D S</au><au>Rácz, I</au><au>Regimbau, T</au><au>Riles, K</au><au>Robinet, F</au><au>Rocchi, A</au><au>Rüdiger, A</au><au>Schuette, D</au><au>Shaddock, D</au><au>Singh, R</au><au>Smith, M</au><au>Stops, D</au><au>Tomlinson, C</au><au>Ugolini, D</au><au>Vajente, G</au><au>Vaulin, R</au><au>Verma, S S</au><au>Wade, M</au><au>Wessels, P</au><au>Wette, K</au><au>Wiesner, K</au><au>Williams, K</au><au>Williams, T</au><au>Winkler, W</au><au>Zucker, M E</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>First all-sky search for continuous gravitational waves from unknown sources in binary systems</atitle><jtitle>arXiv.org</jtitle><date>2014-09-17</date><risdate>2014</risdate><eissn>2331-8422</eissn><abstract>We present the first results of an all-sky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO Science Run and the second and third Virgo Science Runs. The search covers a range of frequencies from 20 Hz to 520 Hz, a range of orbital periods from 2 to ~2,254 h and a frequency- and period-dependent range of frequency modulation depths from 0.277 to 100 mHz. This corresponds to a range of projected semi-major axes of the orbit from ~0.6e-3 ls to ~6,500 ls assuming the orbit of the binary is circular. While no plausible candidate gravitational wave events survive the pipeline, upper limits are set on the analyzed data. The most sensitive 95% confidence upper limit obtained on gravitational wave strain is 2.3e-24 at 217 Hz, assuming the source waves are circularly polarized. Although this search has been optimized for circular binary orbits, the upper limits obtained remain valid for orbital eccentricities as large as 0.9. In addition, upper limits are placed on continuous gravitational wave emission from the low-mass x-ray binary Scorpius X-1 between 20 Hz and 57.25 Hz.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1405.7904</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2014-09 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_1405_7904 |
| source | arXiv.org; Free E- Journals |
| subjects | Algorithms Binary stars Circular polarization Eccentric orbits Frequency modulation Gravitation Gravitational waves Neutron stars Physics - General Relativity and Quantum Cosmology Physics - High Energy Astrophysical Phenomena Searching X ray binaries X ray stars |
| title | First all-sky search for continuous gravitational waves from unknown sources in binary systems |
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